https://gsawg.wiki.ast.cam.ac.uk/api.php?action=feedcontributions&feedformat=atom&user=Chris.davis 2026-05-02T12:58:46Z User contributions MediaWiki 1.35.14 https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Working_groups&diff=1654 2014-03-12T10:52:22Z

<p>Chris.davis: /* GSAWG4: Young Stars */</p> <hr /> <div>Tentative list of Working Groups with people interested to be part of them.<br /> Please email LW if you would like to be added to any of the groups. Soon the pages below will become the workplace for each of the WGs. Email LW if you want to obtain the credentials to edit the wiki pages.<br /> <br /> The numbers indicate the order of joining the group. Volunteers for leading the group are marked in bold.<br /> <br /> [O] - happy to observe<br /> [S] - student<br /> <br /> Link to INT spectroscopy proposal I/2014A/4 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_int.pdf PDF]<br /> <br /> Link to WHT spectroscopy proposal W/2014A/31 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_wht.pdf PDF]<br /> <br /> Link to NTT spectroscopy proposal ID: 093.D-0856 (submitted 1/10/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/d/da/Fuga_ntt.pdf PDF]<br /> <br /> Link to PATT Liverpool Telescope spectroscopy proposal ID: PL14A15 (submitted 4/10/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/3/36/Fugalt.pdf PDF]<br /> <br /> Link to JMU Liverpool Telescope spectroscopy proposal ID: #10 (submitted 4/10/2013) : [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/e/ea/14A-GAIA-JMU.pdf PDF]<br /> <br /> === GSAWG1: Supernovae (Core collapse, 1a) ===<br /> #Simon Clark<br /> #Eran Ofek<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #Sjoert van Velzen [O]<br /> #Patricia Whitelock <br /> #Andrzej Pigulski<br /> #Massimo Turatto<br /> #Lukasz Wyrzykowski [O]<br /> #Michel Dennefeld [O]<br /> #Morgan Fraser [O]<br /> #Lina Tomasella<br /> #Heather Campbell [O]<br /> #Stefano Benetti<br /> #Andrea Pastorello<br /> #Nadia Blagorodnova [O][S]<br /> #'''Nic Walton [O]'''<br /> #Christian Knigge<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Rob Barnsley<br /> #Philip James<br /> #Sergey Koposov<br /> #Valerio A. R. M. Ribeiro<br /> #Ian Skillen<br /> #Giuseppe Altavilla<br /> #Mickael Rigault<br /> #Oliver Vince<br /> #Goran Damljanovic<br /> <br /> === GSAWG2: CVs and XRBs ===<br /> #Simon Clark<br /> #Peter Jonker [O]<br /> #Zbigniew Kolaczkowski<br /> #Ulrich Kolb<br /> #Richard Busuttil<br /> #Boris Gaensicke [O]<br /> #Retha Pretorius<br /> #Andrzej Pigulski<br /> #Stuart P Littlefair [O]<br /> #Chris Copperwheat<br /> #Peter Wheatley [O]<br /> #Stephen Potter<br /> #'''Elme Breedt [O]'''<br /> #Michel Dennefeld [O]<br /> #Danny Steeghs [O]<br /> #Matthew Schurch [O]<br /> #Thomas Wevers [S][O]<br /> #Rob Fender<br /> #Christian Knigge<br /> #Vik Dhillon<br /> #Phil Charles<br /> #Andrew Mason<br /> #Marian Doru Suran<br /> #Dumitru Pricopi<br /> #Alexandru Dumitrescu<br /> #Valerio A. R. M. Ribeiro<br /> #Ian Skillen<br /> <br /> === GSAWG3: Microlensing ===<br /> #Eran Ofek<br /> #Rachel Street<br /> #'''Lukasz Wyrzykowski'''<br /> #Martin Dominik<br /> #Arnaud Cassan<br /> <br /> === [http://wiki.astro.ljmu.ac.uk/YoungTransients/ GSAWG4: Young Stars] ===<br /> ''NOTE: Wiki pages of this WG are password protected. If you want to join this group please email Chris Davis at Liverpool John Moores University''<br /> <br /> #Aleks Scholz [O]<br /> #Zbigniew Kolaczkowski<br /> #'''Chris Davis [O]'''<br /> #Michael Smith<br /> #Dirk Froebrich [O]<br /> #Philip Lucas<br /> #Tigran Magakian<br /> #Suzie Ramsay<br /> #Steve Longmore<br /> #Carlos Contreras<br /> #Tim Naylor [O]<br /> #Darryl Sergison<br /> #Laszlo Szabados<br /> #Cecilia Farina [O]<br /> #Joao Alves<br /> #Tim Gledhill<br /> #Timo Prusti<br /> #Tom Ray<br /> #Tae-Soo Pyo<br /> #Nick Wright<br /> #Hauyu Baobab Liu<br /> #Jochen Eisloeffel<br /> <br /> === GSAWG5: AGNs and TDEs ===<br /> #Paul O'Brien<br /> #Norbert Schartel<br /> #Peter Jonker [O]<br /> #Helene Sol<br /> #Stefanie Komossa<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #'''Sjoert van Velzen''' [O]<br /> #Stephen Potter<br /> #Elme Breedt [O]<br /> #Michel Dennefeld<br /> #Andreja Gomboc<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Ashish Mahabal<br /> #Nic Walton [O]<br /> #Werner Zeilinger<br /> #Carole Mundell<br /> #David Bersier<br /> #Shiho Kobayashi<br /> #Stefano Benetti<br /> #Sergey Koposov<br /> #Oliver Vince<br /> #Goran Damljanovic<br /> #Francois Taris<br /> <br /> === GSAWG6: GRBs ===<br /> #Paul O'Brien<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #David Alexander Kann<br /> #Matthew Schurch [O]<br /> #Andreja Gomboc<br /> #Jure Japelj<br /> #Neil Gehrels<br /> #Carole Mundell<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Shiho Kobayashi<br /> #Stefano Benetti<br /> #Susanna Vergani<br /> <br /> === GSAWG7: Be stars, R CrB stars, other rare events ===<br /> #Simon Clark<br /> #Patrick Tisserand<br /> #Zbigniew Kolaczkowski<br /> #Boris Gaensicke<br /> #Patricia Whitelock<br /> #Andrzej Pigulski<br /> #Peter Wheatley [O]<br /> #Laurent Eyer<br /> #Matthew Schurch<br /> #Laszlo Szabados<br /> #Andrea Pastorello<br /> #Rob Barnsley<br /> #Pavel Koubsky<br /> #Yves Frémat<br /> #Andrew Mason<br /> <br /> === GSAWG8: Gaia Alerts Processing and Infrastructure ===<br /> #'''Simon Hodgkin''' [O]<br /> #Dafydd Wyn Evans<br /> #Francesca De Angeli<br /> #Giorga Busso<br /> #Marco Riello<br /> #Anthony Brown (DPAC chair)<br /> #Nadia Blagorodnova [O][S]<br /> #Patrick Burgess<br /> #Laurent Eyer<br /> #Timo Prusti (ESA: Gaia Project Scientist)<br /> #Sergey Koposov<br /> #Nic Walton (DPAC CU5/CU9 / GST)<br /> <br /> === GSAWG9: Spectroscopic Follow-Up ===<br /> #'''Simon Hodgkin [O]'''<br /> #Lina Tomasella<br /> #Stefanie Komossa<br /> #Danny Steeghs<br /> #Andreja Gomboc<br /> #Cecilia Farina [O]<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Nic Walton [O]<br /> #Chris Davis<br /> #David Bersier<br /> #Werner Zeilinger<br /> #Philippe Bendjoya<br /> #Giuseppe Altavilla<br /> #Mickael Rigault<br /> #Jean-Pierre Rivet<br /> <br /> === GSAWG10: Photometric Follow-Up ===<br /> #'''Lukasz Wyrzykowski'''<br /> #Andreja Gomboc<br /> #Liam K Hardy [O][S]<br /> #Ulrich Kolb [O]<br /> #Peter Wheatley [O]<br /> #Cecilia Farina [O]<br /> #Ashish Mahabal<br /> #Gabor Marschalko [O]<br /> #David Bersier<br /> #Andrzej Pigulski<br /> #Zbyszek Kołaczkowski<br /> #Grzegorz Kopacki<br /> #Przemek Brus<br /> #Dawid Moździerski<br /> #Gabriela Michalska<br /> #Pavel Koubsky<br /> #Philip James<br /> #Sergey Koposov<br /> #Philippe Bendjoya<br /> #Giuseppe Leto<br /> #Giuseppe Altavilla<br /> #Oliver Vince<br /> #Goran Damljanovic<br /> #Jean-Pierre Rivet</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Working_groups&diff=1653 2014-03-11T09:09:05Z

<p>Chris.davis: /* GSAWG4: Young Stars */</p> <hr /> <div>Tentative list of Working Groups with people interested to be part of them.<br /> Please email LW if you would like to be added to any of the groups. Soon the pages below will become the workplace for each of the WGs. Email LW if you want to obtain the credentials to edit the wiki pages.<br /> <br /> The numbers indicate the order of joining the group. Volunteers for leading the group are marked in bold.<br /> <br /> [O] - happy to observe<br /> [S] - student<br /> <br /> Link to INT spectroscopy proposal I/2014A/4 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_int.pdf PDF]<br /> <br /> Link to WHT spectroscopy proposal W/2014A/31 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_wht.pdf PDF]<br /> <br /> Link to NTT spectroscopy proposal ID: 093.D-0856 (submitted 1/10/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/d/da/Fuga_ntt.pdf PDF]<br /> <br /> Link to PATT Liverpool Telescope spectroscopy proposal ID: PL14A15 (submitted 4/10/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/3/36/Fugalt.pdf PDF]<br /> <br /> Link to JMU Liverpool Telescope spectroscopy proposal ID: #10 (submitted 4/10/2013) : [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/e/ea/14A-GAIA-JMU.pdf PDF]<br /> <br /> === GSAWG1: Supernovae (Core collapse, 1a) ===<br /> #Simon Clark<br /> #Eran Ofek<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #Sjoert van Velzen [O]<br /> #Patricia Whitelock <br /> #Andrzej Pigulski<br /> #Massimo Turatto<br /> #Lukasz Wyrzykowski [O]<br /> #Michel Dennefeld [O]<br /> #Morgan Fraser [O]<br /> #Lina Tomasella<br /> #Heather Campbell [O]<br /> #Stefano Benetti<br /> #Andrea Pastorello<br /> #Nadia Blagorodnova [O][S]<br /> #'''Nic Walton [O]'''<br /> #Christian Knigge<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Rob Barnsley<br /> #Philip James<br /> #Sergey Koposov<br /> #Valerio A. R. M. Ribeiro<br /> #Ian Skillen<br /> #Giuseppe Altavilla<br /> #Mickael Rigault<br /> #Oliver Vince<br /> #Goran Damljanovic<br /> <br /> === GSAWG2: CVs and XRBs ===<br /> #Simon Clark<br /> #Peter Jonker [O]<br /> #Zbigniew Kolaczkowski<br /> #Ulrich Kolb<br /> #Richard Busuttil<br /> #Boris Gaensicke [O]<br /> #Retha Pretorius<br /> #Andrzej Pigulski<br /> #Stuart P Littlefair [O]<br /> #Chris Copperwheat<br /> #Peter Wheatley [O]<br /> #Stephen Potter<br /> #'''Elme Breedt [O]'''<br /> #Michel Dennefeld [O]<br /> #Danny Steeghs [O]<br /> #Matthew Schurch [O]<br /> #Thomas Wevers [S][O]<br /> #Rob Fender<br /> #Christian Knigge<br /> #Vik Dhillon<br /> #Phil Charles<br /> #Andrew Mason<br /> #Marian Doru Suran<br /> #Dumitru Pricopi<br /> #Alexandru Dumitrescu<br /> #Valerio A. R. M. Ribeiro<br /> #Ian Skillen<br /> <br /> === GSAWG3: Microlensing ===<br /> #Eran Ofek<br /> #Rachel Street<br /> #'''Lukasz Wyrzykowski'''<br /> #Martin Dominik<br /> #Arnaud Cassan<br /> <br /> === [http://wiki.astro.ljmu.ac.uk/YoungTransients/ GSAWG4: Young Stars] ===<br /> ''NOTE: Wiki pages of this WG are password protected. If you want to join this group please email Chris Davis at Liverpool John Moores University''<br /> <br /> #Aleks Scholz [O]<br /> #Zbigniew Kolaczkowski<br /> #'''Chris Davis [O]'''<br /> #Michael Smith<br /> #Dirk Froebrich [O]<br /> #Philip Lucas<br /> #Tigran Magakian<br /> #Suzie Ramsay<br /> #Steve Longmore<br /> #Carlos Contreras<br /> #Tim Naylor [O]<br /> #Darryl Sergison<br /> #Laszlo Szabados<br /> #Cecilia Farina [O]<br /> #Joao Alves<br /> #Tim Gledhill<br /> #Timo Prusti<br /> #Tom Ray<br /> #Tae-Soo Pyo<br /> #Nick Wright<br /> #Hauyu Baobab Liu<br /> <br /> === GSAWG5: AGNs and TDEs ===<br /> #Paul O'Brien<br /> #Norbert Schartel<br /> #Peter Jonker [O]<br /> #Helene Sol<br /> #Stefanie Komossa<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #'''Sjoert van Velzen''' [O]<br /> #Stephen Potter<br /> #Elme Breedt [O]<br /> #Michel Dennefeld<br /> #Andreja Gomboc<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Ashish Mahabal<br /> #Nic Walton [O]<br /> #Werner Zeilinger<br /> #Carole Mundell<br /> #David Bersier<br /> #Shiho Kobayashi<br /> #Stefano Benetti<br /> #Sergey Koposov<br /> #Oliver Vince<br /> #Goran Damljanovic<br /> #Francois Taris<br /> <br /> === GSAWG6: GRBs ===<br /> #Paul O'Brien<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #David Alexander Kann<br /> #Matthew Schurch [O]<br /> #Andreja Gomboc<br /> #Jure Japelj<br /> #Neil Gehrels<br /> #Carole Mundell<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Shiho Kobayashi<br /> #Stefano Benetti<br /> #Susanna Vergani<br /> <br /> === GSAWG7: Be stars, R CrB stars, other rare events ===<br /> #Simon Clark<br /> #Patrick Tisserand<br /> #Zbigniew Kolaczkowski<br /> #Boris Gaensicke<br /> #Patricia Whitelock<br /> #Andrzej Pigulski<br /> #Peter Wheatley [O]<br /> #Laurent Eyer<br /> #Matthew Schurch<br /> #Laszlo Szabados<br /> #Andrea Pastorello<br /> #Rob Barnsley<br /> #Pavel Koubsky<br /> #Yves Frémat<br /> #Andrew Mason<br /> <br /> === GSAWG8: Gaia Alerts Processing and Infrastructure ===<br /> #'''Simon Hodgkin''' [O]<br /> #Dafydd Wyn Evans<br /> #Francesca De Angeli<br /> #Giorga Busso<br /> #Marco Riello<br /> #Anthony Brown (DPAC chair)<br /> #Nadia Blagorodnova [O][S]<br /> #Patrick Burgess<br /> #Laurent Eyer<br /> #Timo Prusti (ESA: Gaia Project Scientist)<br /> #Sergey Koposov<br /> #Nic Walton (DPAC CU5/CU9 / GST)<br /> <br /> === GSAWG9: Spectroscopic Follow-Up ===<br /> #'''Simon Hodgkin [O]'''<br /> #Lina Tomasella<br /> #Stefanie Komossa<br /> #Danny Steeghs<br /> #Andreja Gomboc<br /> #Cecilia Farina [O]<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Nic Walton [O]<br /> #Chris Davis<br /> #David Bersier<br /> #Werner Zeilinger<br /> #Philippe Bendjoya<br /> #Giuseppe Altavilla<br /> #Mickael Rigault<br /> #Jean-Pierre Rivet<br /> <br /> === GSAWG10: Photometric Follow-Up ===<br /> #'''Lukasz Wyrzykowski'''<br /> #Andreja Gomboc<br /> #Liam K Hardy [O][S]<br /> #Ulrich Kolb [O]<br /> #Peter Wheatley [O]<br /> #Cecilia Farina [O]<br /> #Ashish Mahabal<br /> #Gabor Marschalko [O]<br /> #David Bersier<br /> #Andrzej Pigulski<br /> #Zbyszek Kołaczkowski<br /> #Grzegorz Kopacki<br /> #Przemek Brus<br /> #Dawid Moździerski<br /> #Gabriela Michalska<br /> #Pavel Koubsky<br /> #Philip James<br /> #Sergey Koposov<br /> #Philippe Bendjoya<br /> #Giuseppe Leto<br /> #Giuseppe Altavilla<br /> #Oliver Vince<br /> #Goran Damljanovic<br /> #Jean-Pierre Rivet</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Working_groups&diff=1652 2014-03-11T09:08:21Z

<p>Chris.davis: /* GSAWG4: Young Stars */</p> <hr /> <div>Tentative list of Working Groups with people interested to be part of them.<br /> Please email LW if you would like to be added to any of the groups. Soon the pages below will become the workplace for each of the WGs. Email LW if you want to obtain the credentials to edit the wiki pages.<br /> <br /> The numbers indicate the order of joining the group. Volunteers for leading the group are marked in bold.<br /> <br /> [O] - happy to observe<br /> [S] - student<br /> <br /> Link to INT spectroscopy proposal I/2014A/4 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_int.pdf PDF]<br /> <br /> Link to WHT spectroscopy proposal W/2014A/31 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_wht.pdf PDF]<br /> <br /> Link to NTT spectroscopy proposal ID: 093.D-0856 (submitted 1/10/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/d/da/Fuga_ntt.pdf PDF]<br /> <br /> Link to PATT Liverpool Telescope spectroscopy proposal ID: PL14A15 (submitted 4/10/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/3/36/Fugalt.pdf PDF]<br /> <br /> Link to JMU Liverpool Telescope spectroscopy proposal ID: #10 (submitted 4/10/2013) : [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/e/ea/14A-GAIA-JMU.pdf PDF]<br /> <br /> === GSAWG1: Supernovae (Core collapse, 1a) ===<br /> #Simon Clark<br /> #Eran Ofek<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #Sjoert van Velzen [O]<br /> #Patricia Whitelock <br /> #Andrzej Pigulski<br /> #Massimo Turatto<br /> #Lukasz Wyrzykowski [O]<br /> #Michel Dennefeld [O]<br /> #Morgan Fraser [O]<br /> #Lina Tomasella<br /> #Heather Campbell [O]<br /> #Stefano Benetti<br /> #Andrea Pastorello<br /> #Nadia Blagorodnova [O][S]<br /> #'''Nic Walton [O]'''<br /> #Christian Knigge<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Rob Barnsley<br /> #Philip James<br /> #Sergey Koposov<br /> #Valerio A. R. M. Ribeiro<br /> #Ian Skillen<br /> #Giuseppe Altavilla<br /> #Mickael Rigault<br /> #Oliver Vince<br /> #Goran Damljanovic<br /> <br /> === GSAWG2: CVs and XRBs ===<br /> #Simon Clark<br /> #Peter Jonker [O]<br /> #Zbigniew Kolaczkowski<br /> #Ulrich Kolb<br /> #Richard Busuttil<br /> #Boris Gaensicke [O]<br /> #Retha Pretorius<br /> #Andrzej Pigulski<br /> #Stuart P Littlefair [O]<br /> #Chris Copperwheat<br /> #Peter Wheatley [O]<br /> #Stephen Potter<br /> #'''Elme Breedt [O]'''<br /> #Michel Dennefeld [O]<br /> #Danny Steeghs [O]<br /> #Matthew Schurch [O]<br /> #Thomas Wevers [S][O]<br /> #Rob Fender<br /> #Christian Knigge<br /> #Vik Dhillon<br /> #Phil Charles<br /> #Andrew Mason<br /> #Marian Doru Suran<br /> #Dumitru Pricopi<br /> #Alexandru Dumitrescu<br /> #Valerio A. R. M. Ribeiro<br /> #Ian Skillen<br /> <br /> === GSAWG3: Microlensing ===<br /> #Eran Ofek<br /> #Rachel Street<br /> #'''Lukasz Wyrzykowski'''<br /> #Martin Dominik<br /> #Arnaud Cassan<br /> <br /> === [http://wiki.astro.ljmu.ac.uk/YoungTransients/ GSAWG4: Young Stars] ===<br /> ''NOTE: Wiki pages of this WG are password protected. If you want to join this group please email Chris Davis''<br /> <br /> #Aleks Scholz [O]<br /> #Zbigniew Kolaczkowski<br /> #'''Chris Davis [O]'''<br /> #Michael Smith<br /> #Dirk Froebrich [O]<br /> #Philip Lucas<br /> #Tigran Magakian<br /> #Suzie Ramsay<br /> #Steve Longmore<br /> #Carlos Contreras<br /> #Tim Naylor [O]<br /> #Darryl Sergison<br /> #Laszlo Szabados<br /> #Cecilia Farina [O]<br /> #Joao Alves<br /> #Tim Gledhill<br /> #Timo Prusti<br /> #Tom Ray<br /> #Tae-Soo Pyo<br /> #Nick Wright<br /> #Hauyu Baobab Liu<br /> <br /> === GSAWG5: AGNs and TDEs ===<br /> #Paul O'Brien<br /> #Norbert Schartel<br /> #Peter Jonker [O]<br /> #Helene Sol<br /> #Stefanie Komossa<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #'''Sjoert van Velzen''' [O]<br /> #Stephen Potter<br /> #Elme Breedt [O]<br /> #Michel Dennefeld<br /> #Andreja Gomboc<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Ashish Mahabal<br /> #Nic Walton [O]<br /> #Werner Zeilinger<br /> #Carole Mundell<br /> #David Bersier<br /> #Shiho Kobayashi<br /> #Stefano Benetti<br /> #Sergey Koposov<br /> #Oliver Vince<br /> #Goran Damljanovic<br /> #Francois Taris<br /> <br /> === GSAWG6: GRBs ===<br /> #Paul O'Brien<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #David Alexander Kann<br /> #Matthew Schurch [O]<br /> #Andreja Gomboc<br /> #Jure Japelj<br /> #Neil Gehrels<br /> #Carole Mundell<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Shiho Kobayashi<br /> #Stefano Benetti<br /> #Susanna Vergani<br /> <br /> === GSAWG7: Be stars, R CrB stars, other rare events ===<br /> #Simon Clark<br /> #Patrick Tisserand<br /> #Zbigniew Kolaczkowski<br /> #Boris Gaensicke<br /> #Patricia Whitelock<br /> #Andrzej Pigulski<br /> #Peter Wheatley [O]<br /> #Laurent Eyer<br /> #Matthew Schurch<br /> #Laszlo Szabados<br /> #Andrea Pastorello<br /> #Rob Barnsley<br /> #Pavel Koubsky<br /> #Yves Frémat<br /> #Andrew Mason<br /> <br /> === GSAWG8: Gaia Alerts Processing and Infrastructure ===<br /> #'''Simon Hodgkin''' [O]<br /> #Dafydd Wyn Evans<br /> #Francesca De Angeli<br /> #Giorga Busso<br /> #Marco Riello<br /> #Anthony Brown (DPAC chair)<br /> #Nadia Blagorodnova [O][S]<br /> #Patrick Burgess<br /> #Laurent Eyer<br /> #Timo Prusti (ESA: Gaia Project Scientist)<br /> #Sergey Koposov<br /> #Nic Walton (DPAC CU5/CU9 / GST)<br /> <br /> === GSAWG9: Spectroscopic Follow-Up ===<br /> #'''Simon Hodgkin [O]'''<br /> #Lina Tomasella<br /> #Stefanie Komossa<br /> #Danny Steeghs<br /> #Andreja Gomboc<br /> #Cecilia Farina [O]<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Nic Walton [O]<br /> #Chris Davis<br /> #David Bersier<br /> #Werner Zeilinger<br /> #Philippe Bendjoya<br /> #Giuseppe Altavilla<br /> #Mickael Rigault<br /> #Jean-Pierre Rivet<br /> <br /> === GSAWG10: Photometric Follow-Up ===<br /> #'''Lukasz Wyrzykowski'''<br /> #Andreja Gomboc<br /> #Liam K Hardy [O][S]<br /> #Ulrich Kolb [O]<br /> #Peter Wheatley [O]<br /> #Cecilia Farina [O]<br /> #Ashish Mahabal<br /> #Gabor Marschalko [O]<br /> #David Bersier<br /> #Andrzej Pigulski<br /> #Zbyszek Kołaczkowski<br /> #Grzegorz Kopacki<br /> #Przemek Brus<br /> #Dawid Moździerski<br /> #Gabriela Michalska<br /> #Pavel Koubsky<br /> #Philip James<br /> #Sergey Koposov<br /> #Philippe Bendjoya<br /> #Giuseppe Leto<br /> #Giuseppe Altavilla<br /> #Oliver Vince<br /> #Goran Damljanovic<br /> #Jean-Pierre Rivet</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Working_groups&diff=1642 2013-12-19T09:31:35Z

<p>Chris.davis: /* GSAWG4: Young Stars */</p> <hr /> <div>Tentative list of Working Groups with people interested to be part of them.<br /> Please email LW if you would like to be added to any of the groups. Soon the pages below will become the workplace for each of the WGs. Email LW if you want to obtain the credentials to edit the wiki pages.<br /> <br /> The numbers indicate the order of joining the group. Volunteers for leading the group are marked in bold.<br /> <br /> [O] - happy to observe<br /> [S] - student<br /> <br /> Link to INT spectroscopy proposal I/2014A/4 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_int.pdf PDF]<br /> <br /> Link to WHT spectroscopy proposal W/2014A/31 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_wht.pdf PDF]<br /> <br /> Link to NTT spectroscopy proposal ID: 093.D-0856 (submitted 1/10/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/d/da/Fuga_ntt.pdf PDF]<br /> <br /> Link to PATT Liverpool Telescope spectroscopy proposal ID: PL14A15 (submitted 4/10/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/3/36/Fugalt.pdf PDF]<br /> <br /> Link to JMU Liverpool Telescope spectroscopy proposal ID: #10 (submitted 4/10/2013) : [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/e/ea/14A-GAIA-JMU.pdf PDF]<br /> <br /> === GSAWG1: Supernovae (Core collapse, 1a) ===<br /> #Simon Clark<br /> #Eran Ofek<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #Sjoert van Velzen [O]<br /> #Patricia Whitelock <br /> #Andrzej Pigulski<br /> #Massimo Turatto<br /> #Lukasz Wyrzykowski [O]<br /> #Michel Dennefeld [O]<br /> #Morgan Fraser [O]<br /> #Lina Tomasella<br /> #Heather Campbell [O]<br /> #Stefano Benetti<br /> #Andrea Pastorello<br /> #Nadia Blagorodnova [O][S]<br /> #'''Nic Walton [O]'''<br /> #Christian Knigge<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Rob Barnsley<br /> #Philip James<br /> #Sergey Koposov<br /> #Valerio A. R. M. Ribeiro<br /> #Ian Skillen<br /> <br /> === GSAWG2: CVs and XRBs ===<br /> #Simon Clark<br /> #Peter Jonker [O]<br /> #Zbigniew Kolaczkowski<br /> #Ulrich Kolb<br /> #Richard Busuttil<br /> #Boris Gaensicke [O]<br /> #Retha Pretorius<br /> #Andrzej Pigulski<br /> #Stuart P Littlefair [O]<br /> #Chris Copperwheat<br /> #Peter Wheatley [O]<br /> #Stephen Potter<br /> #'''Elme Breedt [O]'''<br /> #Michel Dennefeld [O]<br /> #Danny Steeghs [O]<br /> #Matthew Schurch [O]<br /> #Thomas Wevers [S][O]<br /> #Rob Fender<br /> #Christian Knigge<br /> #Vik Dhillon<br /> #Phil Charles<br /> #Andrew Mason<br /> #Marian Doru Suran<br /> #Dumitru Pricopi<br /> #Alexandru Dumitrescu<br /> #Valerio A. R. M. Ribeiro<br /> #Ian Skillen<br /> <br /> === GSAWG3: Microlensing ===<br /> #Eran Ofek<br /> #Rachel Street<br /> #'''Lukasz Wyrzykowski'''<br /> #Martin Dominik<br /> #Arnaud Cassan<br /> <br /> === GSAWG4: Young Stars ===<br /> #Aleks Scholz [O]<br /> #Zbigniew Kolaczkowski<br /> #'''Chris Davis [O]'''<br /> #Michael Smith<br /> #Dirk Froebrich [O]<br /> #Philip Lucas<br /> #Tigran Magakian<br /> #Suzie Ramsay<br /> #Steve Longmore<br /> #Carlos Contreras<br /> #Tim Naylor [O]<br /> #Darryl Sergison<br /> #Laszlo Szabados<br /> #Cecilia Farina [O]<br /> #Joao Alves<br /> #Tim Gledhill<br /> #Timo Prusti<br /> #Tom Ray<br /> <br /> === GSAWG5: AGNs and TDEs ===<br /> #Paul O'Brien<br /> #Norbert Schartel<br /> #Peter Jonker [O]<br /> #Helene Sol<br /> #Stefanie Komossa<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #'''Sjoert van Velzen''' [O]<br /> #Stephen Potter<br /> #Elme Breedt [O]<br /> #Michel Dennefeld<br /> #Andreja Gomboc<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Ashish Mahabal<br /> #Nic Walton [O]<br /> #Werner Zeilinger<br /> #Carole Mundell<br /> #David Bersier<br /> #Shiho Kobayashi<br /> #Stefano Benetti<br /> #Sergey Koposov<br /> <br /> === GSAWG6: GRBs ===<br /> #Paul O'Brien<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #David Alexander Kann<br /> #Matthew Schurch [O]<br /> #Andreja Gomboc<br /> #Jure Japelj<br /> #Neil Gehrels<br /> #Carole Mundell<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Shiho Kobayashi<br /> #Stefano Benetti<br /> #Susanna Vergani<br /> <br /> === GSAWG7: Be stars, R CrB stars, other rare events ===<br /> #Simon Clark<br /> #Patrick Tisserand<br /> #Zbigniew Kolaczkowski<br /> #Boris Gaensicke<br /> #Patricia Whitelock<br /> #Andrzej Pigulski<br /> #Peter Wheatley [O]<br /> #Laurent Eyer<br /> #Matthew Schurch<br /> #Laszlo Szabados<br /> #Andrea Pastorello<br /> #Rob Barnsley<br /> #Pavel Koubsky<br /> #Yves Frémat<br /> #Andrew Mason<br /> <br /> === GSAWG8: Gaia Alerts Processing and Infrastructure ===<br /> #'''Simon Hodgkin''' [O]<br /> #Dafydd Wyn Evans<br /> #Francesca De Angeli<br /> #Giorga Busso<br /> #Marco Riello<br /> #Anthony Brown (DPAC chair)<br /> #Nadia Blagorodnova [O][S]<br /> #Patrick Burgess<br /> #Laurent Eyer<br /> #Timo Prusti (ESA: Gaia Project Scientist)<br /> #Sergey Koposov<br /> <br /> === GSAWG9: Spectroscopic Follow-Up ===<br /> #'''Simon Hodgkin [O]'''<br /> #Lina Tomasella<br /> #Stefanie Komossa<br /> #Danny Steeghs<br /> #Andreja Gomboc<br /> #Cecilia Farina [O]<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Nic Walton [O]<br /> #Chris Davis<br /> #David Bersier<br /> #Werner Zeilinger<br /> #Philippe Bendjoya<br /> <br /> === GSAWG10: Photometric Follow-Up ===<br /> #'''Lukasz Wyrzykowski'''<br /> #Andreja Gomboc<br /> #Liam K Hardy [O][S]<br /> #Ulrich Kolb [O]<br /> #Peter Wheatley [O]<br /> #Cecilia Farina [O]<br /> #Ashish Mahabal<br /> #Gabor Marschalko [O]<br /> #David Bersier<br /> #Andrzej Pigulski<br /> #Zbyszek Kołaczkowski<br /> #Grzegorz Kopacki<br /> #Przemek Brus<br /> #Dawid Moździerski<br /> #Gabriela Michalska<br /> #Pavel Koubsky<br /> #Philip James<br /> #Sergey Koposov<br /> #Philippe Bendjoya<br /> #Giuseppe Leto</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Working_groups&diff=1641 2013-12-19T09:31:13Z

<p>Chris.davis: /* GSAWG4: Young Stars */</p> <hr /> <div>Tentative list of Working Groups with people interested to be part of them.<br /> Please email LW if you would like to be added to any of the groups. Soon the pages below will become the workplace for each of the WGs. Email LW if you want to obtain the credentials to edit the wiki pages.<br /> <br /> The numbers indicate the order of joining the group. Volunteers for leading the group are marked in bold.<br /> <br /> [O] - happy to observe<br /> [S] - student<br /> <br /> Link to INT spectroscopy proposal I/2014A/4 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_int.pdf PDF]<br /> <br /> Link to WHT spectroscopy proposal W/2014A/31 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_wht.pdf PDF]<br /> <br /> Link to NTT spectroscopy proposal ID: 093.D-0856 (submitted 1/10/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/d/da/Fuga_ntt.pdf PDF]<br /> <br /> Link to PATT Liverpool Telescope spectroscopy proposal ID: PL14A15 (submitted 4/10/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/3/36/Fugalt.pdf PDF]<br /> <br /> Link to JMU Liverpool Telescope spectroscopy proposal ID: #10 (submitted 4/10/2013) : [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/e/ea/14A-GAIA-JMU.pdf PDF]<br /> <br /> === GSAWG1: Supernovae (Core collapse, 1a) ===<br /> #Simon Clark<br /> #Eran Ofek<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #Sjoert van Velzen [O]<br /> #Patricia Whitelock <br /> #Andrzej Pigulski<br /> #Massimo Turatto<br /> #Lukasz Wyrzykowski [O]<br /> #Michel Dennefeld [O]<br /> #Morgan Fraser [O]<br /> #Lina Tomasella<br /> #Heather Campbell [O]<br /> #Stefano Benetti<br /> #Andrea Pastorello<br /> #Nadia Blagorodnova [O][S]<br /> #'''Nic Walton [O]'''<br /> #Christian Knigge<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Rob Barnsley<br /> #Philip James<br /> #Sergey Koposov<br /> #Valerio A. R. M. Ribeiro<br /> #Ian Skillen<br /> <br /> === GSAWG2: CVs and XRBs ===<br /> #Simon Clark<br /> #Peter Jonker [O]<br /> #Zbigniew Kolaczkowski<br /> #Ulrich Kolb<br /> #Richard Busuttil<br /> #Boris Gaensicke [O]<br /> #Retha Pretorius<br /> #Andrzej Pigulski<br /> #Stuart P Littlefair [O]<br /> #Chris Copperwheat<br /> #Peter Wheatley [O]<br /> #Stephen Potter<br /> #'''Elme Breedt [O]'''<br /> #Michel Dennefeld [O]<br /> #Danny Steeghs [O]<br /> #Matthew Schurch [O]<br /> #Thomas Wevers [S][O]<br /> #Rob Fender<br /> #Christian Knigge<br /> #Vik Dhillon<br /> #Phil Charles<br /> #Andrew Mason<br /> #Marian Doru Suran<br /> #Dumitru Pricopi<br /> #Alexandru Dumitrescu<br /> #Valerio A. R. M. Ribeiro<br /> #Ian Skillen<br /> <br /> === GSAWG3: Microlensing ===<br /> #Eran Ofek<br /> #Rachel Street<br /> #'''Lukasz Wyrzykowski'''<br /> #Martin Dominik<br /> #Arnaud Cassan<br /> <br /> === GSAWG4: Young Stars ===<br /> #Aleks Scholz [O]<br /> #Zbigniew Kolaczkowski<br /> #Chris Davis [O]<br /> #Michael Smith<br /> #Dirk Froebrich [O]<br /> #Philip Lucas<br /> #Tigran Magakian<br /> #Suzie Ramsay<br /> #Steve Longmore<br /> #Carlos Contreras<br /> #Tim Naylor [O]<br /> #Darryl Sergison<br /> #Laszlo Szabados<br /> #Cecilia Farina [O]<br /> #Joao Alves<br /> #Tim Gledhill<br /> #Timo Prusti<br /> #Tom Ray<br /> <br /> === GSAWG5: AGNs and TDEs ===<br /> #Paul O'Brien<br /> #Norbert Schartel<br /> #Peter Jonker [O]<br /> #Helene Sol<br /> #Stefanie Komossa<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #'''Sjoert van Velzen''' [O]<br /> #Stephen Potter<br /> #Elme Breedt [O]<br /> #Michel Dennefeld<br /> #Andreja Gomboc<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Ashish Mahabal<br /> #Nic Walton [O]<br /> #Werner Zeilinger<br /> #Carole Mundell<br /> #David Bersier<br /> #Shiho Kobayashi<br /> #Stefano Benetti<br /> #Sergey Koposov<br /> <br /> === GSAWG6: GRBs ===<br /> #Paul O'Brien<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #David Alexander Kann<br /> #Matthew Schurch [O]<br /> #Andreja Gomboc<br /> #Jure Japelj<br /> #Neil Gehrels<br /> #Carole Mundell<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Shiho Kobayashi<br /> #Stefano Benetti<br /> #Susanna Vergani<br /> <br /> === GSAWG7: Be stars, R CrB stars, other rare events ===<br /> #Simon Clark<br /> #Patrick Tisserand<br /> #Zbigniew Kolaczkowski<br /> #Boris Gaensicke<br /> #Patricia Whitelock<br /> #Andrzej Pigulski<br /> #Peter Wheatley [O]<br /> #Laurent Eyer<br /> #Matthew Schurch<br /> #Laszlo Szabados<br /> #Andrea Pastorello<br /> #Rob Barnsley<br /> #Pavel Koubsky<br /> #Yves Frémat<br /> #Andrew Mason<br /> <br /> === GSAWG8: Gaia Alerts Processing and Infrastructure ===<br /> #'''Simon Hodgkin''' [O]<br /> #Dafydd Wyn Evans<br /> #Francesca De Angeli<br /> #Giorga Busso<br /> #Marco Riello<br /> #Anthony Brown (DPAC chair)<br /> #Nadia Blagorodnova [O][S]<br /> #Patrick Burgess<br /> #Laurent Eyer<br /> #Timo Prusti (ESA: Gaia Project Scientist)<br /> #Sergey Koposov<br /> <br /> === GSAWG9: Spectroscopic Follow-Up ===<br /> #'''Simon Hodgkin [O]'''<br /> #Lina Tomasella<br /> #Stefanie Komossa<br /> #Danny Steeghs<br /> #Andreja Gomboc<br /> #Cecilia Farina [O]<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Nic Walton [O]<br /> #Chris Davis<br /> #David Bersier<br /> #Werner Zeilinger<br /> #Philippe Bendjoya<br /> <br /> === GSAWG10: Photometric Follow-Up ===<br /> #'''Lukasz Wyrzykowski'''<br /> #Andreja Gomboc<br /> #Liam K Hardy [O][S]<br /> #Ulrich Kolb [O]<br /> #Peter Wheatley [O]<br /> #Cecilia Farina [O]<br /> #Ashish Mahabal<br /> #Gabor Marschalko [O]<br /> #David Bersier<br /> #Andrzej Pigulski<br /> #Zbyszek Kołaczkowski<br /> #Grzegorz Kopacki<br /> #Przemek Brus<br /> #Dawid Moździerski<br /> #Gabriela Michalska<br /> #Pavel Koubsky<br /> #Philip James<br /> #Sergey Koposov<br /> #Philippe Bendjoya<br /> #Giuseppe Leto</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Working_groups&diff=1640 2013-12-19T09:30:09Z

<p>Chris.davis: /* GSAWG4: Young Stars */</p> <hr /> <div>Tentative list of Working Groups with people interested to be part of them.<br /> Please email LW if you would like to be added to any of the groups. Soon the pages below will become the workplace for each of the WGs. Email LW if you want to obtain the credentials to edit the wiki pages.<br /> <br /> The numbers indicate the order of joining the group. Volunteers for leading the group are marked in bold.<br /> <br /> [O] - happy to observe<br /> [S] - student<br /> <br /> Link to INT spectroscopy proposal I/2014A/4 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_int.pdf PDF]<br /> <br /> Link to WHT spectroscopy proposal W/2014A/31 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_wht.pdf PDF]<br /> <br /> Link to NTT spectroscopy proposal ID: 093.D-0856 (submitted 1/10/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/d/da/Fuga_ntt.pdf PDF]<br /> <br /> Link to PATT Liverpool Telescope spectroscopy proposal ID: PL14A15 (submitted 4/10/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/3/36/Fugalt.pdf PDF]<br /> <br /> Link to JMU Liverpool Telescope spectroscopy proposal ID: #10 (submitted 4/10/2013) : [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/e/ea/14A-GAIA-JMU.pdf PDF]<br /> <br /> === GSAWG1: Supernovae (Core collapse, 1a) ===<br /> #Simon Clark<br /> #Eran Ofek<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #Sjoert van Velzen [O]<br /> #Patricia Whitelock <br /> #Andrzej Pigulski<br /> #Massimo Turatto<br /> #Lukasz Wyrzykowski [O]<br /> #Michel Dennefeld [O]<br /> #Morgan Fraser [O]<br /> #Lina Tomasella<br /> #Heather Campbell [O]<br /> #Stefano Benetti<br /> #Andrea Pastorello<br /> #Nadia Blagorodnova [O][S]<br /> #'''Nic Walton [O]'''<br /> #Christian Knigge<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Rob Barnsley<br /> #Philip James<br /> #Sergey Koposov<br /> #Valerio A. R. M. Ribeiro<br /> #Ian Skillen<br /> <br /> === GSAWG2: CVs and XRBs ===<br /> #Simon Clark<br /> #Peter Jonker [O]<br /> #Zbigniew Kolaczkowski<br /> #Ulrich Kolb<br /> #Richard Busuttil<br /> #Boris Gaensicke [O]<br /> #Retha Pretorius<br /> #Andrzej Pigulski<br /> #Stuart P Littlefair [O]<br /> #Chris Copperwheat<br /> #Peter Wheatley [O]<br /> #Stephen Potter<br /> #'''Elme Breedt [O]'''<br /> #Michel Dennefeld [O]<br /> #Danny Steeghs [O]<br /> #Matthew Schurch [O]<br /> #Thomas Wevers [S][O]<br /> #Rob Fender<br /> #Christian Knigge<br /> #Vik Dhillon<br /> #Phil Charles<br /> #Andrew Mason<br /> #Marian Doru Suran<br /> #Dumitru Pricopi<br /> #Alexandru Dumitrescu<br /> #Valerio A. R. M. Ribeiro<br /> #Ian Skillen<br /> <br /> === GSAWG3: Microlensing ===<br /> #Eran Ofek<br /> #Rachel Street<br /> #'''Lukasz Wyrzykowski'''<br /> #Martin Dominik<br /> #Arnaud Cassan<br /> <br /> === GSAWG4: Young Stars ===<br /> #Aleks Scholz [O]<br /> #Zbigniew Kolaczkowski<br /> #Chris Davis<br /> #Michael Smith<br /> #Dirk Froebrich [O]<br /> #Philip Lucas<br /> #Tigran Magakian<br /> #Suzie Ramsay<br /> #Steve Longmore<br /> #Carlos Contreras<br /> #Tim Naylor [O]<br /> #Darryl Sergison<br /> #Laszlo Szabados<br /> #Cecilia Farina [O]<br /> #Joao Alves<br /> #Tim Gledhill<br /> #Timo Prusti<br /> #Tom Ray<br /> <br /> === GSAWG5: AGNs and TDEs ===<br /> #Paul O'Brien<br /> #Norbert Schartel<br /> #Peter Jonker [O]<br /> #Helene Sol<br /> #Stefanie Komossa<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #'''Sjoert van Velzen''' [O]<br /> #Stephen Potter<br /> #Elme Breedt [O]<br /> #Michel Dennefeld<br /> #Andreja Gomboc<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Ashish Mahabal<br /> #Nic Walton [O]<br /> #Werner Zeilinger<br /> #Carole Mundell<br /> #David Bersier<br /> #Shiho Kobayashi<br /> #Stefano Benetti<br /> #Sergey Koposov<br /> <br /> === GSAWG6: GRBs ===<br /> #Paul O'Brien<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #David Alexander Kann<br /> #Matthew Schurch [O]<br /> #Andreja Gomboc<br /> #Jure Japelj<br /> #Neil Gehrels<br /> #Carole Mundell<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Shiho Kobayashi<br /> #Stefano Benetti<br /> #Susanna Vergani<br /> <br /> === GSAWG7: Be stars, R CrB stars, other rare events ===<br /> #Simon Clark<br /> #Patrick Tisserand<br /> #Zbigniew Kolaczkowski<br /> #Boris Gaensicke<br /> #Patricia Whitelock<br /> #Andrzej Pigulski<br /> #Peter Wheatley [O]<br /> #Laurent Eyer<br /> #Matthew Schurch<br /> #Laszlo Szabados<br /> #Andrea Pastorello<br /> #Rob Barnsley<br /> #Pavel Koubsky<br /> #Yves Frémat<br /> #Andrew Mason<br /> <br /> === GSAWG8: Gaia Alerts Processing and Infrastructure ===<br /> #'''Simon Hodgkin''' [O]<br /> #Dafydd Wyn Evans<br /> #Francesca De Angeli<br /> #Giorga Busso<br /> #Marco Riello<br /> #Anthony Brown (DPAC chair)<br /> #Nadia Blagorodnova [O][S]<br /> #Patrick Burgess<br /> #Laurent Eyer<br /> #Timo Prusti (ESA: Gaia Project Scientist)<br /> #Sergey Koposov<br /> <br /> === GSAWG9: Spectroscopic Follow-Up ===<br /> #'''Simon Hodgkin [O]'''<br /> #Lina Tomasella<br /> #Stefanie Komossa<br /> #Danny Steeghs<br /> #Andreja Gomboc<br /> #Cecilia Farina [O]<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Nic Walton [O]<br /> #Chris Davis<br /> #David Bersier<br /> #Werner Zeilinger<br /> #Philippe Bendjoya<br /> <br /> === GSAWG10: Photometric Follow-Up ===<br /> #'''Lukasz Wyrzykowski'''<br /> #Andreja Gomboc<br /> #Liam K Hardy [O][S]<br /> #Ulrich Kolb [O]<br /> #Peter Wheatley [O]<br /> #Cecilia Farina [O]<br /> #Ashish Mahabal<br /> #Gabor Marschalko [O]<br /> #David Bersier<br /> #Andrzej Pigulski<br /> #Zbyszek Kołaczkowski<br /> #Grzegorz Kopacki<br /> #Przemek Brus<br /> #Dawid Moździerski<br /> #Gabriela Michalska<br /> #Pavel Koubsky<br /> #Philip James<br /> #Sergey Koposov<br /> #Philippe Bendjoya<br /> #Giuseppe Leto</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Working_groups&diff=1639 2013-12-19T09:29:56Z

<p>Chris.davis: /* GSAWG4: Young Stars */</p> <hr /> <div>Tentative list of Working Groups with people interested to be part of them.<br /> Please email LW if you would like to be added to any of the groups. Soon the pages below will become the workplace for each of the WGs. Email LW if you want to obtain the credentials to edit the wiki pages.<br /> <br /> The numbers indicate the order of joining the group. Volunteers for leading the group are marked in bold.<br /> <br /> [O] - happy to observe<br /> [S] - student<br /> <br /> Link to INT spectroscopy proposal I/2014A/4 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_int.pdf PDF]<br /> <br /> Link to WHT spectroscopy proposal W/2014A/31 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_wht.pdf PDF]<br /> <br /> Link to NTT spectroscopy proposal ID: 093.D-0856 (submitted 1/10/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/d/da/Fuga_ntt.pdf PDF]<br /> <br /> Link to PATT Liverpool Telescope spectroscopy proposal ID: PL14A15 (submitted 4/10/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/3/36/Fugalt.pdf PDF]<br /> <br /> Link to JMU Liverpool Telescope spectroscopy proposal ID: #10 (submitted 4/10/2013) : [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/images/e/ea/14A-GAIA-JMU.pdf PDF]<br /> <br /> === GSAWG1: Supernovae (Core collapse, 1a) ===<br /> #Simon Clark<br /> #Eran Ofek<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #Sjoert van Velzen [O]<br /> #Patricia Whitelock <br /> #Andrzej Pigulski<br /> #Massimo Turatto<br /> #Lukasz Wyrzykowski [O]<br /> #Michel Dennefeld [O]<br /> #Morgan Fraser [O]<br /> #Lina Tomasella<br /> #Heather Campbell [O]<br /> #Stefano Benetti<br /> #Andrea Pastorello<br /> #Nadia Blagorodnova [O][S]<br /> #'''Nic Walton [O]'''<br /> #Christian Knigge<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Rob Barnsley<br /> #Philip James<br /> #Sergey Koposov<br /> #Valerio A. R. M. Ribeiro<br /> #Ian Skillen<br /> <br /> === GSAWG2: CVs and XRBs ===<br /> #Simon Clark<br /> #Peter Jonker [O]<br /> #Zbigniew Kolaczkowski<br /> #Ulrich Kolb<br /> #Richard Busuttil<br /> #Boris Gaensicke [O]<br /> #Retha Pretorius<br /> #Andrzej Pigulski<br /> #Stuart P Littlefair [O]<br /> #Chris Copperwheat<br /> #Peter Wheatley [O]<br /> #Stephen Potter<br /> #'''Elme Breedt [O]'''<br /> #Michel Dennefeld [O]<br /> #Danny Steeghs [O]<br /> #Matthew Schurch [O]<br /> #Thomas Wevers [S][O]<br /> #Rob Fender<br /> #Christian Knigge<br /> #Vik Dhillon<br /> #Phil Charles<br /> #Andrew Mason<br /> #Marian Doru Suran<br /> #Dumitru Pricopi<br /> #Alexandru Dumitrescu<br /> #Valerio A. R. M. Ribeiro<br /> #Ian Skillen<br /> <br /> === GSAWG3: Microlensing ===<br /> #Eran Ofek<br /> #Rachel Street<br /> #'''Lukasz Wyrzykowski'''<br /> #Martin Dominik<br /> #Arnaud Cassan<br /> <br /> === GSAWG4: Young Stars ===<br /> #Aleks Scholz [O]<br /> #Zbigniew Kolaczkowski<br /> #Chris Davis<br /> #Michael Smith<br /> #Dirk Froebrich [O]<br /> #Philip Lucas<br /> #Tigran Magakian<br /> #Suzie Ramsay<br /> #Steve Longmore<br /> #Carlos Contreras<br /> #Tim Naylor [O]<br /> #Darryl Sergison<br /> #Laszlo Szabados<br /> #Cecilia Farina [O]<br /> #Joao Alves<br /> #Tim Gledhill<br /> #Timo Prusti<br /> *Tom Ray<br /> <br /> === GSAWG5: AGNs and TDEs ===<br /> #Paul O'Brien<br /> #Norbert Schartel<br /> #Peter Jonker [O]<br /> #Helene Sol<br /> #Stefanie Komossa<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #'''Sjoert van Velzen''' [O]<br /> #Stephen Potter<br /> #Elme Breedt [O]<br /> #Michel Dennefeld<br /> #Andreja Gomboc<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Ashish Mahabal<br /> #Nic Walton [O]<br /> #Werner Zeilinger<br /> #Carole Mundell<br /> #David Bersier<br /> #Shiho Kobayashi<br /> #Stefano Benetti<br /> #Sergey Koposov<br /> <br /> === GSAWG6: GRBs ===<br /> #Paul O'Brien<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #David Alexander Kann<br /> #Matthew Schurch [O]<br /> #Andreja Gomboc<br /> #Jure Japelj<br /> #Neil Gehrels<br /> #Carole Mundell<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Shiho Kobayashi<br /> #Stefano Benetti<br /> #Susanna Vergani<br /> <br /> === GSAWG7: Be stars, R CrB stars, other rare events ===<br /> #Simon Clark<br /> #Patrick Tisserand<br /> #Zbigniew Kolaczkowski<br /> #Boris Gaensicke<br /> #Patricia Whitelock<br /> #Andrzej Pigulski<br /> #Peter Wheatley [O]<br /> #Laurent Eyer<br /> #Matthew Schurch<br /> #Laszlo Szabados<br /> #Andrea Pastorello<br /> #Rob Barnsley<br /> #Pavel Koubsky<br /> #Yves Frémat<br /> #Andrew Mason<br /> <br /> === GSAWG8: Gaia Alerts Processing and Infrastructure ===<br /> #'''Simon Hodgkin''' [O]<br /> #Dafydd Wyn Evans<br /> #Francesca De Angeli<br /> #Giorga Busso<br /> #Marco Riello<br /> #Anthony Brown (DPAC chair)<br /> #Nadia Blagorodnova [O][S]<br /> #Patrick Burgess<br /> #Laurent Eyer<br /> #Timo Prusti (ESA: Gaia Project Scientist)<br /> #Sergey Koposov<br /> <br /> === GSAWG9: Spectroscopic Follow-Up ===<br /> #'''Simon Hodgkin [O]'''<br /> #Lina Tomasella<br /> #Stefanie Komossa<br /> #Danny Steeghs<br /> #Andreja Gomboc<br /> #Cecilia Farina [O]<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Nic Walton [O]<br /> #Chris Davis<br /> #David Bersier<br /> #Werner Zeilinger<br /> #Philippe Bendjoya<br /> <br /> === GSAWG10: Photometric Follow-Up ===<br /> #'''Lukasz Wyrzykowski'''<br /> #Andreja Gomboc<br /> #Liam K Hardy [O][S]<br /> #Ulrich Kolb [O]<br /> #Peter Wheatley [O]<br /> #Cecilia Farina [O]<br /> #Ashish Mahabal<br /> #Gabor Marschalko [O]<br /> #David Bersier<br /> #Andrzej Pigulski<br /> #Zbyszek Kołaczkowski<br /> #Grzegorz Kopacki<br /> #Przemek Brus<br /> #Dawid Moździerski<br /> #Gabriela Michalska<br /> #Pavel Koubsky<br /> #Philip James<br /> #Sergey Koposov<br /> #Philippe Bendjoya<br /> #Giuseppe Leto</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Working_groups&diff=1586 2013-09-17T10:11:21Z

<p>Chris.davis: /* GSAWG4: Young Stars */</p> <hr /> <div>Tentative list of Working Groups with people interested to be part of them.<br /> Please email LW if you would like to be added to any of the groups. Soon the pages below will become the workplace for each of the WGs. Email LW if you want to obtain the credentials to edit the wiki pages.<br /> <br /> The numbers indicate the order of joining the group. Volunteers for leading the group are marked in bold.<br /> <br /> [O] - happy to observe<br /> [S] - student<br /> <br /> Link to INT spectroscopy proposal I/2014A/4 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_int.pdf PDF]<br /> <br /> Link to WHT spectroscopy proposal W/2014A/31 (submitted 15/9/2013): [http://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/File:Fuga_wht.pdf PDF]<br /> <br /> === GSAWG1: Supernovae (Core collapse, 1a) ===<br /> #Simon Clark<br /> #Eran Ofek<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #Sjoert van Velzen [O]<br /> #Patricia Whitelock <br /> #Andrzej Pigulski<br /> #Massimo Turatto<br /> #Lukasz Wyrzykowski [O]<br /> #Morgan Fraser [O]<br /> #Lina Tomasella<br /> #Heather Campbell [O]<br /> #Stefano Benetti<br /> #Andrea Pastorello<br /> #Nadia Blagorodnova [O][S]<br /> #Nic Walton [O]<br /> #Christian Knigge<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Rob Barnsley<br /> <br /> === GSAWG2: CVs and XRBs ===<br /> #Simon Clark<br /> #Peter Jonker [O]<br /> #Zbigniew Kolaczkowski<br /> #Ulrich Kolb<br /> #Richard Busuttil<br /> #Boris Gaensicke [O]<br /> #Retha Pretorius<br /> #Andrzej Pigulski<br /> #Stuart P Littlefair [O]<br /> #Chris Copperwheat<br /> #Peter Wheatley [O]<br /> #Stephen Potter<br /> #'''Elme Breedt [O]'''<br /> #Danny Steeghs [O]<br /> #Matthew Schurch [O]<br /> #Thomas Wevers [S][O]<br /> #Rob Fender<br /> #Christian Knigge<br /> <br /> === GSAWG3: Microlensing ===<br /> #Eran Ofek<br /> #Rachel Street<br /> #Lukasz Wyrzykowski<br /> #Martin Dominik<br /> <br /> === GSAWG4: Young Stars ===<br /> #Aleks Scholz [O]<br /> #Zbigniew Kolaczkowski<br /> #Chris Davis<br /> #Michael Smith<br /> #Dirk Froebrich<br /> #Philip Lucas<br /> #Tigran Magakian<br /> #Suzie Ramsay<br /> #Steve Longmore<br /> #Carlos Contreras<br /> #Tim Naylor [O]<br /> #Darryl Sergison<br /> #Laszlo Szabados<br /> #Cecilia Farina [O]<br /> #Joao Alves<br /> #Tim Gledhill<br /> <br /> === GSAWG5: AGNs and TDEs ===<br /> #Paul O'Brien<br /> #Norbert Schartel<br /> #Peter Jonker [O]<br /> #Helene Sol<br /> #Stefanie Komossa<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #'''Sjoert van Velzen''' [O]<br /> #Stephen Potter<br /> #Elme Breedt [O]<br /> #Andreja Gomboc<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Ashish Mahabal<br /> #Nic Walton [O]<br /> #Werner Zeilinger<br /> #Carole Mundell<br /> #David Bersier<br /> #Shiho Kobayashi<br /> <br /> === GSAWG6: GRBs ===<br /> #Paul O'Brien<br /> #Stephen Smartt<br /> #Mark Sullivan [O]<br /> #David Alexander Kann<br /> #Matthew Schurch [O]<br /> #Andreja Gomboc<br /> #Jure Japelj<br /> #Neil Gehrels<br /> #Carole Mundell<br /> #Paolo Mazzali<br /> #David Bersier<br /> #Shiho Kobayashi<br /> <br /> === GSAWG7: Be stars, R CrB stars, other rare events ===<br /> #Simon Clark<br /> #Patrick Tisserand<br /> #Zbigniew Kolaczkowski<br /> #Boris Gaensicke<br /> #Patricia Whitelock<br /> #Andrzej Pigulski<br /> #Peter Wheatley [O]<br /> #Laurent Eyer<br /> #Matthew Schurch<br /> #Laszlo Szabados<br /> #Andrea Pastorello<br /> #Rob Barnsley<br /> #Pavel Koubsky<br /> <br /> === GSAWG8: Gaia Alerts Processing and Infrastructure ===<br /> #'''Simon Hodgkin''' [O]<br /> #Dafydd Wyn Evans<br /> #Francesca De Angeli<br /> #Giorga Busso<br /> #Marco Riello<br /> #Anthony Brown (DPAC chair)<br /> #Nadia Blagorodnova [O][S]<br /> #Patrick Burgess<br /> #Laurent Eyer<br /> <br /> === GSAWG9: Spectroscopic Follow-Up ===<br /> #'''Simon Hodgkin (PI INT spectroscopy programme) [O]'''<br /> #Lina Tomasella<br /> #Stefanie Komossa<br /> #Danny Steeghs<br /> #Andreja Gomboc<br /> #Cecilia Farina [O]<br /> #Morgan Fraser [O]<br /> #Nadia Blagorodnova [O][S]<br /> #Nic Walton [O]<br /> <br /> === GSAWG10: Photometric Follow-Up ===<br /> #'''Lukasz Wyrzykowski'''<br /> #Andreja Gomboc<br /> #Liam K Hardy [O][S]<br /> #Ulrich Kolb [O]<br /> #Peter Wheatley [O]<br /> #Cecilia Farina [O]<br /> #Ashish Mahabal<br /> #Gabor Marschalko [O]<br /> #David Bersier<br /> #Andrzej Pigulski<br /> #Zbyszek Kołaczkowski<br /> #Grzegorz Kopacki<br /> #Przemek Brus<br /> #Dawid Moździerski<br /> #Gabriela Michalska<br /> #Pavel Koubsky</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Working_groups&diff=1528 2013-08-27T07:36:56Z

<p>Chris.davis: /* GSAWG4: Young Stars */</p> <hr /> <div>Tentative list of Working Groups with people interested to be part of them.<br /> Please email LW if you would like to be added to any of the groups. Soon the pages below will become the workplace for each of the WGs. Email LW if you want to obtain the credentials to edit the wiki pages.<br /> <br /> === GSAWG1: Supernovae (Core collapse, 1a) ===<br /> #Simon Clark<br /> #Eran Ofek<br /> #Stephen Smartt<br /> #Mark Sullivan<br /> #Sjoert van Velzen<br /> #Patricia Whitelock<br /> #Andrzej Pigulski<br /> #Massimo Turatto<br /> #Lukasz Wyrzykowski<br /> <br /> <br /> === GSAWG2: CVs and XRBs ===<br /> #Simon Clark<br /> #Peter Jonker<br /> #Zbigniew Kolaczkowski<br /> #Ulrich Kolb<br /> #Richard Busuttil<br /> #Boris Gaensicke<br /> #Retha Pretorius<br /> #Andrzej Pigulski<br /> #Stuart P Littlefair<br /> #Chris Copperwheat<br /> #Peter Wheatley<br /> #Stephen Potter<br /> <br /> === GSAWG3: Microlensing ===<br /> #Eran Ofek<br /> #Rachel Street<br /> #Lukasz Wyrzykowski<br /> #Martin Dominik<br /> <br /> === GSAWG4: Young Stars ===<br /> #Aleks Scholz<br /> #Zbigniew Kolaczkowski<br /> #Chris Davis<br /> #Michael Smith<br /> #Dirk Froebrich<br /> #Philip Lucas<br /> #Tigran Magakian<br /> #Suzie Ramsay<br /> #Steve Longmore<br /> #Carlos Contreras<br /> #Tim Naylor<br /> #Darryl Sergison<br /> <br /> === GSAWG5: AGNs and TDEs ===<br /> #Paul O'Brien<br /> #Norbert Schartel<br /> #Peter Jonker<br /> #Helene Sol<br /> #Stefanie Komossa<br /> #Stephen Smartt<br /> #Mark Sullivan<br /> #Sjoert van Velzen<br /> #Stephen Potter<br /> <br /> === GSAWG6: GRBs ===<br /> #Paul O'Brien<br /> #Stephen Smartt<br /> #Mark Sullivan<br /> #David Alexander Kann<br /> <br /> === GSAWG7: Be stars, R CrB stars, other rare events ===<br /> #Simon Clark<br /> #Patrick Tisserand<br /> #Zbigniew Kolaczkowski<br /> #Boris Gaensicke<br /> #Patricia Whitelock<br /> #Andrzej Pigulski<br /> #Peter Wheatley</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Working_groups&diff=1524 2013-08-02T10:04:41Z

<p>Chris.davis: /* GSAWG4: Young Stars */</p> <hr /> <div>Tentative list of Working Groups with people interested to be part of them.<br /> Please email LW if you would like to be added to any of the groups. Soon the pages below will become the workplace for each of the WGs. Email LW if you want to obtain the credentials to edit the wiki pages.<br /> <br /> === GSAWG1: Supernovae (Core collapse, 1a) ===<br /> #Simon Clark<br /> #Eran Ofek<br /> #Stephen Smartt<br /> #Mark Sullivan<br /> #Sjoert van Velzen<br /> #Patricia Whitelock<br /> #Andrzej Pigulski<br /> <br /> === GSAWG2: CVs and XRBs ===<br /> #Simon Clark<br /> #Peter Jonker<br /> #Zbigniew Kolaczkowski<br /> #Ulrich Kolb<br /> #Richard Busuttil<br /> #Boris Gaensicke<br /> #Retha Pretorius<br /> #Andrzej Pigulski<br /> #Stuart P Littlefair<br /> #Chris Copperwheat<br /> #Peter Wheatley<br /> <br /> === GSAWG3: Microlensing ===<br /> #Eran Ofek<br /> #Rachel Street<br /> #Lukasz Wyrzykowski<br /> #Martin Dominik<br /> <br /> === GSAWG4: Young Stars ===<br /> #Aleks Scholz<br /> #Zbigniew Kolaczkowski<br /> #Chris J. Davis<br /> #Michael Smith<br /> #Dirk Froebrich<br /> #Philip Lucas<br /> #Tigran Magakian<br /> #Suzie Ramsay<br /> #Steve Longmore<br /> <br /> === GSAWG5: AGNs and TDEs ===<br /> #Paul O'Brien<br /> #Norbert Schartel<br /> #Peter Jonker<br /> #Helene Sol<br /> #Stefanie Komossa<br /> #Stephen Smartt<br /> #Mark Sullivan<br /> #Sjoert van Velzen<br /> <br /> === GSAWG6: GRBs ===<br /> #Paul O'Brien<br /> #Stephen Smartt<br /> #Mark Sullivan<br /> <br /> === GSAWG7: Be stars, R CrB stars, other rare events ===<br /> #Simon Clark<br /> #Patrick Tisserand<br /> #Zbigniew Kolaczkowski<br /> #Boris Gaensicke<br /> #Patricia Whitelock<br /> #Andrzej Pigulski<br /> #Peter Wheatley</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers&diff=1519 2013-07-26T15:14:36Z

<p>Chris.davis: /* Possible triggers for Science Alerts */</p> <hr /> <div>''' Please expand this section with your favourite types of possible alerts. The most useful information would be the number statistics, amplitude and timescale, example light curve, spectrum and the reasoning for an rapid alert.'''<br /> <br /> ===Possible triggers for Science Alerts===<br /> <br /> * [[Triggers:Asteroids | Asteroids]]<br /> <br /> * [[Triggers:Be | Be-type stars]]<br /> <br /> * [[Triggers:CVs | Cataclysmic Variables (CVs)]]<br /> <br /> * [[Triggers:CNe | Classical novae]]<br /> <br /> * [[Triggers:DNe | Dwarf novae]]<br /> <br /> * [[Triggers:GRBs | Gamma Ray Bursts Optical Counterparts]]<br /> <br /> * [[Triggers:LensedSNe | Gravitationally lensed supernovae]]<br /> <br /> * [[Triggers:LBVs | Luminous Blue Variables]]<br /> <br /> * [[Triggers:Flares | M-dwarf flares]]<br /> <br /> * [[Triggers:Microlensing | Microlensing events]]<br /> <br /> * [[Triggers:RCrB | R Coronae Borealis type variables (dimming objects)]]<br /> <br /> * [[Triggers:Supernovae | Supernovae]]<br /> <br /> * [[Triggers:TTau | T Tauri stars and other Young variables]]<br /> <br /> ** [[Triggers:FUOri | Eruptive young stellar objects]]<br /> <br /> ** [[Triggers:YSOecl | Eclipsing young stellar objects]]<br /> <br /> * [[Triggers:XBs | X-ray binaries (XBs)]]<br /> <br /> <br /> * [[Triggers:Other | Other rare transients]]<br /> <br /> * [[Triggers:Theoretical | Exotic/theoretical events]]<br /> <br /> == Table of transients ==<br /> This table is based on [http://arxiv.org/abs/0906.5355 Rau et al. 2009] on Palomar Transient Factory (PTF).<br /> MR is an absolute magnitude in R, tau is time of a decline by 2 mag.<br /> Note, these are not all the types of transites Gaia will detect.<br /> <br /> {| border=&quot;1&quot; cellspacing=&quot;0&quot; cellpadding=&quot;5&quot; align=&quot;center&quot;<br /> ! Class<br /> ! MR<br /> ! tau<br /> ! Universal rate<br /> ! Gaia rate<br /> |- <br /> | Dwarf Novae<br /> | 9..4<br /> | 3..20<br /> | &lt;math&gt;3\times10^{-5} \textrm{pc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Classical Novae<br /> | -5..-10<br /> |2..100<br /> |&lt;math&gt;2\times10^{-10} \textrm{yr}^{-1}\textrm{L}_{\odot,K}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Luminous Red Novae<br /> | -10..-14<br /> |20..60<br /> |&lt;math&gt;1.5\times10^{-13} \textrm{yr}^{-1}\textrm{L}_{\odot,K}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Fallback SNe<br /> | -4..-21<br /> |0.5..2<br /> |&lt;math&gt;10^{-13} \textrm{yr}^{-1}\textrm{L}_{\odot,K}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Macronovae<br /> | -13..-15<br /> |0.3..3<br /> |&lt;math&gt;10^{-4..-8} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |SN .Ia<br /> | -15..-17<br /> |2..5<br /> |&lt;math&gt;(4..10)\times 10^{-6} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |SNe Ia<br /> | -17..-19.5<br /> |30..70<br /> |&lt;math&gt;3\times 10^{-5} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Tidal disruption flares<br /> | -15..-19<br /> |30..350<br /> |&lt;math&gt;10^{-6} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Core-collapse SNe<br /> | -14..-21<br /> |20..300<br /> |&lt;math&gt;5\times 10^{-5} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Luminous SNe<br /> | -19..-23<br /> |50..400<br /> |&lt;math&gt;10^{-7} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Orphan afterglows (SGRB)<br /> | -14..-18<br /> |5..15<br /> |&lt;math&gt;3\times 10^{-7..-9} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Orphan afterglows (LGRB)<br /> | -22..-26<br /> |2..15<br /> |&lt;math&gt;3\times 10^{-7..-9} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |On-axis LGRB afterglows<br /> | ..-37<br /> |1..15<br /> |&lt;math&gt;4\times 10^{-10} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |}<br /> <br /> ----<br /> == CMD of selected variables and transients ==<br /> CMD paths of various types of variable stars, including Be stars, R CrB and V4334 Sgr. From [http://arxiv.org/abs/0907.4090 Spano et al. 2009]<br /> <br /> [[File:VariablesPathsCMDLMC.png|650px]]<br /> <br /> ----<br /> == Time scales and amplitudes ==<br /> [[File:Kulkarni-absmag-timescale.png|400px|left|thumb|Absolute magnitude vs timescale of novae, supernovae and some of new transients. From Kulkarni (2009).]]<br /> <br /> [[File:plot_transients_tau_ampl.png|400px]]<br /> [[File:plot_transients_trise_ampl.png|400px]]<br /> [[File:plot_transients_tdecline_ampl.png|400px]]<br /> [[File:plot_transients_trise_tdecline.png|400px]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers&diff=1518 2013-07-26T15:14:13Z

<p>Chris.davis: /* Possible triggers for Science Alerts */</p> <hr /> <div>''' Please expand this section with your favourite types of possible alerts. The most useful information would be the number statistics, amplitude and timescale, example light curve, spectrum and the reasoning for an rapid alert.'''<br /> <br /> ===Possible triggers for Science Alerts===<br /> <br /> * [[Triggers:Asteroids | Asteroids]]<br /> <br /> * [[Triggers:Be | Be-type stars]]<br /> <br /> * [[Triggers:CVs | Cataclysmic Variables (CVs)]]<br /> <br /> * [[Triggers:CNe | Classical novae]]<br /> <br /> * [[Triggers:DNe | Dwarf novae]]<br /> <br /> * [[Triggers:FUOri | Eruptive young stellar objects]]<br /> <br /> * [[Triggers:YSOecl | Eclipsing young stellar objects]]<br /> <br /> * [[Triggers:GRBs | Gamma Ray Bursts Optical Counterparts]]<br /> <br /> * [[Triggers:LensedSNe | Gravitationally lensed supernovae]]<br /> <br /> * [[Triggers:LBVs | Luminous Blue Variables]]<br /> <br /> * [[Triggers:Flares | M-dwarf flares]]<br /> <br /> * [[Triggers:Microlensing | Microlensing events]]<br /> <br /> * [[Triggers:RCrB | R Coronae Borealis type variables (dimming objects)]]<br /> <br /> * [[Triggers:Supernovae | Supernovae]]<br /> <br /> * [[Triggers:TTau | T Tauri stars and other Young variables]]<br /> <br /> ** [[Triggers:FUOri | Eruptive young stellar objects]]<br /> <br /> ** [[Triggers:YSOecl | Eclipsing young stellar objects]]<br /> <br /> * [[Triggers:XBs | X-ray binaries (XBs)]]<br /> <br /> <br /> * [[Triggers:Other | Other rare transients]]<br /> <br /> * [[Triggers:Theoretical | Exotic/theoretical events]]<br /> <br /> == Table of transients ==<br /> This table is based on [http://arxiv.org/abs/0906.5355 Rau et al. 2009] on Palomar Transient Factory (PTF).<br /> MR is an absolute magnitude in R, tau is time of a decline by 2 mag.<br /> Note, these are not all the types of transites Gaia will detect.<br /> <br /> {| border=&quot;1&quot; cellspacing=&quot;0&quot; cellpadding=&quot;5&quot; align=&quot;center&quot;<br /> ! Class<br /> ! MR<br /> ! tau<br /> ! Universal rate<br /> ! Gaia rate<br /> |- <br /> | Dwarf Novae<br /> | 9..4<br /> | 3..20<br /> | &lt;math&gt;3\times10^{-5} \textrm{pc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Classical Novae<br /> | -5..-10<br /> |2..100<br /> |&lt;math&gt;2\times10^{-10} \textrm{yr}^{-1}\textrm{L}_{\odot,K}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Luminous Red Novae<br /> | -10..-14<br /> |20..60<br /> |&lt;math&gt;1.5\times10^{-13} \textrm{yr}^{-1}\textrm{L}_{\odot,K}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Fallback SNe<br /> | -4..-21<br /> |0.5..2<br /> |&lt;math&gt;10^{-13} \textrm{yr}^{-1}\textrm{L}_{\odot,K}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Macronovae<br /> | -13..-15<br /> |0.3..3<br /> |&lt;math&gt;10^{-4..-8} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |SN .Ia<br /> | -15..-17<br /> |2..5<br /> |&lt;math&gt;(4..10)\times 10^{-6} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |SNe Ia<br /> | -17..-19.5<br /> |30..70<br /> |&lt;math&gt;3\times 10^{-5} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Tidal disruption flares<br /> | -15..-19<br /> |30..350<br /> |&lt;math&gt;10^{-6} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Core-collapse SNe<br /> | -14..-21<br /> |20..300<br /> |&lt;math&gt;5\times 10^{-5} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Luminous SNe<br /> | -19..-23<br /> |50..400<br /> |&lt;math&gt;10^{-7} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Orphan afterglows (SGRB)<br /> | -14..-18<br /> |5..15<br /> |&lt;math&gt;3\times 10^{-7..-9} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |Orphan afterglows (LGRB)<br /> | -22..-26<br /> |2..15<br /> |&lt;math&gt;3\times 10^{-7..-9} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |On-axis LGRB afterglows<br /> | ..-37<br /> |1..15<br /> |&lt;math&gt;4\times 10^{-10} \textrm{Mpc}^{-3} \textrm{yr}^{-1}&lt;/math&gt;<br /> |<br /> |-<br /> |}<br /> <br /> ----<br /> == CMD of selected variables and transients ==<br /> CMD paths of various types of variable stars, including Be stars, R CrB and V4334 Sgr. From [http://arxiv.org/abs/0907.4090 Spano et al. 2009]<br /> <br /> [[File:VariablesPathsCMDLMC.png|650px]]<br /> <br /> ----<br /> == Time scales and amplitudes ==<br /> [[File:Kulkarni-absmag-timescale.png|400px|left|thumb|Absolute magnitude vs timescale of novae, supernovae and some of new transients. From Kulkarni (2009).]]<br /> <br /> [[File:plot_transients_tau_ampl.png|400px]]<br /> [[File:plot_transients_trise_ampl.png|400px]]<br /> [[File:plot_transients_tdecline_ampl.png|400px]]<br /> [[File:plot_transients_trise_tdecline.png|400px]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1517 2013-07-26T15:10:05Z

<p>Chris.davis: /* FU-Ori and EX-Ori and other outbursts */</p> <hr /> <div>= T Tauri stars and other young variables and transients =<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars (TTSs) are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; yr), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;), pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989]. They are optically visible (spectral type F,G,K,M) and their spectral energy distributions possess a modest excess in the near- and mid-IR, although the slope of their SED in the IR is still negative. Classical TTSs (Class II Young Stellar Objects) exhibit strong forbidden emission lines from ionised oxygen, sulphure, iron, etc., and they are often associated with Herbig-Haro jets; weak-lined TTSs (Class III YSOs) are essentially line-free. <br /> <br /> Class I YSOs possess a very strong IR excess (flat or positive spectral indices), are embedded, and are brighter in the near- and mid-IR bands. There is some statistical evidence that Class I YSOs - protostars - are the progenitors of TTSs; they are typically less abundant than Class II YSOs, are more likely to coincide with dark clouds and molecular cores, and may be much younger (&lt; 100,000 yr).<br /> <br /> T Tauri stars are known to vary on periods of days, weeks, and months. Causes include episodic accretion events, warped disk occultations, the transit of dark spots in the photosphere.<br /> <br /> == Relevant characteristics of TTSs ==<br /> <br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> == Spectral features ==<br /> <br /> * Strong Balmer emission lines<br /> * Strong forbidden emission lines; [OI], [SII], [NII], etc.<br /> * Lithium absorption<br /> * P Cygni profiles (due to outflowing gas); inverse P Cygni in some cases<br /> <br /> == FU-Ori, EX-Ori and other outbursts ==<br /> <br /> Some young pre-main-sequence stars have exhibited quite drastic episodic variations. <br /> 1-3 mag eruptions have been observed in several objects (e.g. EX Lup, DR Tau), while<br /> more spectacular eruptions corresponding to a brightening of 3-6 mag have been measured<br /> in FU Orionis type variables (FU-ors). A dozen young stars are now characterised as FUors. Most have<br /> been observed to rise 3-5 mag in brightness in less than one<br /> year; V1515 Cyg is the only known example to require a decade to rise<br /> to visual maximum. Note, however, that the historical light curves for many systems<br /> are poorly documented.<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|450px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|450px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]<br /> <br /> [[File:TTSvsFUor-spec.jpeg|900px|center|thumb|A comparison of red spectra for FU Ori and DG Tau]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1516 2013-07-26T13:48:42Z

<p>Chris.davis: /* Spectral features */</p> <hr /> <div>= T Tauri stars and other young variables and transients =<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars (TTSs) are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; yr), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;), pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989]. They are optically visible (spectral type F,G,K,M) and their spectral energy distributions possess a modest excess in the near- and mid-IR, although the slope of their SED in the IR is still negative. Classical TTSs (Class II Young Stellar Objects) exhibit strong forbidden emission lines from ionised oxygen, sulphure, iron, etc., and they are often associated with Herbig-Haro jets; weak-lined TTSs (Class III YSOs) are essentially line-free. <br /> <br /> Class I YSOs possess a very strong IR excess (flat or positive spectral indices), are embedded, and are brighter in the near- and mid-IR bands. There is some statistical evidence that Class I YSOs - protostars - are the progenitors of TTSs; they are typically less abundant than Class II YSOs, are more likely to coincide with dark clouds and molecular cores, and may be much younger (&lt; 100,000 yr).<br /> <br /> T Tauri stars are known to vary on periods of days, weeks, and months. Causes include episodic accretion events, warped disk occultations, the transit of dark spots in the photosphere.<br /> <br /> == Relevant characteristics of TTSs ==<br /> <br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> == Spectral features ==<br /> <br /> * Strong Balmer emission lines<br /> * Strong forbidden emission lines; [OI], [SII], [NII], etc.<br /> * Lithium absorption<br /> * P Cygni profiles (due to outflowing gas); inverse P Cygni in some cases<br /> <br /> == FU-Ori and EX-Ori and other outbursts ==<br /> <br /> Some young pre-main-sequence stars have exhibited quite drastic episodic variations. <br /> 1-3 mag eruptions have been observed in several objects (e.g. EX Lup, DR Tau), while<br /> more spectacular eruptions corresponding to a brightening of 3-6 mag have been measured<br /> in FU Orionis type variables (FU-ors). A dozen young stars are now characterised as FUors. Most have<br /> been observed to rise 3-5 mag in brightness in less than one<br /> year; V1515 Cyg is the only known example to require a decade to rise<br /> to visual maximum. Note, however, that the historical light curves for many systems<br /> are poorly documented.<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|450px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|450px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]<br /> <br /> [[File:TTSvsFUor-spec.jpeg|900px|center|thumb|A comparison of red spectra for FU Ori and DG Tau]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1515 2013-07-26T13:48:09Z

<p>Chris.davis: /* Relevant characteristics of TTSs: */</p> <hr /> <div>= T Tauri stars and other young variables and transients =<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars (TTSs) are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; yr), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;), pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989]. They are optically visible (spectral type F,G,K,M) and their spectral energy distributions possess a modest excess in the near- and mid-IR, although the slope of their SED in the IR is still negative. Classical TTSs (Class II Young Stellar Objects) exhibit strong forbidden emission lines from ionised oxygen, sulphure, iron, etc., and they are often associated with Herbig-Haro jets; weak-lined TTSs (Class III YSOs) are essentially line-free. <br /> <br /> Class I YSOs possess a very strong IR excess (flat or positive spectral indices), are embedded, and are brighter in the near- and mid-IR bands. There is some statistical evidence that Class I YSOs - protostars - are the progenitors of TTSs; they are typically less abundant than Class II YSOs, are more likely to coincide with dark clouds and molecular cores, and may be much younger (&lt; 100,000 yr).<br /> <br /> T Tauri stars are known to vary on periods of days, weeks, and months. Causes include episodic accretion events, warped disk occultations, the transit of dark spots in the photosphere.<br /> <br /> == Relevant characteristics of TTSs ==<br /> <br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> == Spectral features ==<br /> <br /> * Strong Balmer emission lines<br /> * Strong forbidden emission lines; [OI], [SII], [NII], etc.<br /> * Lithium absorption<br /> * P Cygni profiles<br /> <br /> == FU-Ori and EX-Ori and other outbursts ==<br /> <br /> Some young pre-main-sequence stars have exhibited quite drastic episodic variations. <br /> 1-3 mag eruptions have been observed in several objects (e.g. EX Lup, DR Tau), while<br /> more spectacular eruptions corresponding to a brightening of 3-6 mag have been measured<br /> in FU Orionis type variables (FU-ors). A dozen young stars are now characterised as FUors. Most have<br /> been observed to rise 3-5 mag in brightness in less than one<br /> year; V1515 Cyg is the only known example to require a decade to rise<br /> to visual maximum. Note, however, that the historical light curves for many systems<br /> are poorly documented.<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|450px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|450px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]<br /> <br /> [[File:TTSvsFUor-spec.jpeg|900px|center|thumb|A comparison of red spectra for FU Ori and DG Tau]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1514 2013-07-26T13:47:53Z

<p>Chris.davis: /* Spectral features: */</p> <hr /> <div>= T Tauri stars and other young variables and transients =<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars (TTSs) are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; yr), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;), pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989]. They are optically visible (spectral type F,G,K,M) and their spectral energy distributions possess a modest excess in the near- and mid-IR, although the slope of their SED in the IR is still negative. Classical TTSs (Class II Young Stellar Objects) exhibit strong forbidden emission lines from ionised oxygen, sulphure, iron, etc., and they are often associated with Herbig-Haro jets; weak-lined TTSs (Class III YSOs) are essentially line-free. <br /> <br /> Class I YSOs possess a very strong IR excess (flat or positive spectral indices), are embedded, and are brighter in the near- and mid-IR bands. There is some statistical evidence that Class I YSOs - protostars - are the progenitors of TTSs; they are typically less abundant than Class II YSOs, are more likely to coincide with dark clouds and molecular cores, and may be much younger (&lt; 100,000 yr).<br /> <br /> T Tauri stars are known to vary on periods of days, weeks, and months. Causes include episodic accretion events, warped disk occultations, the transit of dark spots in the photosphere.<br /> <br /> == Relevant characteristics of TTSs: ==<br /> <br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> == Spectral features ==<br /> <br /> * Strong Balmer emission lines<br /> * Strong forbidden emission lines; [OI], [SII], [NII], etc.<br /> * Lithium absorption<br /> * P Cygni profiles<br /> <br /> == FU-Ori and EX-Ori and other outbursts ==<br /> <br /> Some young pre-main-sequence stars have exhibited quite drastic episodic variations. <br /> 1-3 mag eruptions have been observed in several objects (e.g. EX Lup, DR Tau), while<br /> more spectacular eruptions corresponding to a brightening of 3-6 mag have been measured<br /> in FU Orionis type variables (FU-ors). A dozen young stars are now characterised as FUors. Most have<br /> been observed to rise 3-5 mag in brightness in less than one<br /> year; V1515 Cyg is the only known example to require a decade to rise<br /> to visual maximum. Note, however, that the historical light curves for many systems<br /> are poorly documented.<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|450px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|450px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]<br /> <br /> [[File:TTSvsFUor-spec.jpeg|900px|center|thumb|A comparison of red spectra for FU Ori and DG Tau]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=File:TTSvsFUor-spec.jpeg&diff=1513 2013-07-26T13:45:36Z

<p>Chris.davis: </p> <hr /> <div></div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1512 2013-07-26T13:45:23Z

<p>Chris.davis: /* FU-Ori and EX-Ori and other outbursts */</p> <hr /> <div>= T Tauri stars and other young variables and transients =<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars (TTSs) are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; yr), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;), pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989]. They are optically visible (spectral type F,G,K,M) and their spectral energy distributions possess a modest excess in the near- and mid-IR, although the slope of their SED in the IR is still negative. Classical TTSs (Class II Young Stellar Objects) exhibit strong forbidden emission lines from ionised oxygen, sulphure, iron, etc., and they are often associated with Herbig-Haro jets; weak-lined TTSs (Class III YSOs) are essentially line-free. <br /> <br /> Class I YSOs possess a very strong IR excess (flat or positive spectral indices), are embedded, and are brighter in the near- and mid-IR bands. There is some statistical evidence that Class I YSOs - protostars - are the progenitors of TTSs; they are typically less abundant than Class II YSOs, are more likely to coincide with dark clouds and molecular cores, and may be much younger (&lt; 100,000 yr).<br /> <br /> T Tauri stars are known to vary on periods of days, weeks, and months. Causes include episodic accretion events, warped disk occultations, the transit of dark spots in the photosphere.<br /> <br /> == Relevant characteristics of TTSs: ==<br /> <br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> == Spectral features: ==<br /> <br /> * Strong Balmer emission lines<br /> * Strong forbidden emission lines; [OI], [SII], [NII], etc.<br /> * Lithium absorption<br /> * P Cygni profiles<br /> <br /> == FU-Ori and EX-Ori and other outbursts ==<br /> <br /> Some young pre-main-sequence stars have exhibited quite drastic episodic variations. <br /> 1-3 mag eruptions have been observed in several objects (e.g. EX Lup, DR Tau), while<br /> more spectacular eruptions corresponding to a brightening of 3-6 mag have been measured<br /> in FU Orionis type variables (FU-ors). A dozen young stars are now characterised as FUors. Most have<br /> been observed to rise 3-5 mag in brightness in less than one<br /> year; V1515 Cyg is the only known example to require a decade to rise<br /> to visual maximum. Note, however, that the historical light curves for many systems<br /> are poorly documented.<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|450px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|450px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]<br /> <br /> [[File:TTSvsFUor-spec.jpeg|900px|center|thumb|A comparison of red spectra for FU Ori and DG Tau]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1511 2013-07-26T13:14:52Z

<p>Chris.davis: /* Spectral features: */</p> <hr /> <div>= T Tauri stars and other young variables and transients =<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars (TTSs) are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; yr), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;), pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989]. They are optically visible (spectral type F,G,K,M) and their spectral energy distributions possess a modest excess in the near- and mid-IR, although the slope of their SED in the IR is still negative. Classical TTSs (Class II Young Stellar Objects) exhibit strong forbidden emission lines from ionised oxygen, sulphure, iron, etc., and they are often associated with Herbig-Haro jets; weak-lined TTSs (Class III YSOs) are essentially line-free. <br /> <br /> Class I YSOs possess a very strong IR excess (flat or positive spectral indices), are embedded, and are brighter in the near- and mid-IR bands. There is some statistical evidence that Class I YSOs - protostars - are the progenitors of TTSs; they are typically less abundant than Class II YSOs, are more likely to coincide with dark clouds and molecular cores, and may be much younger (&lt; 100,000 yr).<br /> <br /> T Tauri stars are known to vary on periods of days, weeks, and months. Causes include episodic accretion events, warped disk occultations, the transit of dark spots in the photosphere.<br /> <br /> == Relevant characteristics of TTSs: ==<br /> <br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> == Spectral features: ==<br /> <br /> * Strong Balmer emission lines<br /> * Strong forbidden emission lines; [OI], [SII], [NII], etc.<br /> * Lithium absorption<br /> * P Cygni profiles<br /> <br /> == FU-Ori and EX-Ori and other outbursts ==<br /> <br /> Some young pre-main-sequence stars have exhibited quite drastic episodic variations. <br /> 1-3 mag eruptions have been observed in several objects (e.g. EX Lup, DR Tau), while<br /> more spectacular eruptions corresponding to a brightening of 3-6 mag have been measured<br /> in FU Orionis type variables (FU-ors). A dozen young stars are now characterised as FUors. Most have<br /> been observed to rise 3-5 mag in brightness in less than one<br /> year; V1515 Cyg is the only known example to require a decade to rise<br /> to visual maximum. Note, however, that the historical light curves for many systems<br /> are poorly documented.<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|450px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|450px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1510 2013-07-26T13:02:20Z

<p>Chris.davis: /* T Tauri stars and other young variables and transients */</p> <hr /> <div>= T Tauri stars and other young variables and transients =<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars (TTSs) are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; yr), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;), pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989]. They are optically visible (spectral type F,G,K,M) and their spectral energy distributions possess a modest excess in the near- and mid-IR, although the slope of their SED in the IR is still negative. Classical TTSs (Class II Young Stellar Objects) exhibit strong forbidden emission lines from ionised oxygen, sulphure, iron, etc., and they are often associated with Herbig-Haro jets; weak-lined TTSs (Class III YSOs) are essentially line-free. <br /> <br /> Class I YSOs possess a very strong IR excess (flat or positive spectral indices), are embedded, and are brighter in the near- and mid-IR bands. There is some statistical evidence that Class I YSOs - protostars - are the progenitors of TTSs; they are typically less abundant than Class II YSOs, are more likely to coincide with dark clouds and molecular cores, and may be much younger (&lt; 100,000 yr).<br /> <br /> T Tauri stars are known to vary on periods of days, weeks, and months. Causes include episodic accretion events, warped disk occultations, the transit of dark spots in the photosphere.<br /> <br /> == Relevant characteristics of TTSs: ==<br /> <br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> == Spectral features: ==<br /> <br /> * Strong Balmer emission lines<br /> * Lithium absorption<br /> * P Cygni profiles <br /> <br /> == FU-Ori and EX-Ori and other outbursts ==<br /> <br /> Some young pre-main-sequence stars have exhibited quite drastic episodic variations. <br /> 1-3 mag eruptions have been observed in several objects (e.g. EX Lup, DR Tau), while<br /> more spectacular eruptions corresponding to a brightening of 3-6 mag have been measured<br /> in FU Orionis type variables (FU-ors). A dozen young stars are now characterised as FUors. Most have<br /> been observed to rise 3-5 mag in brightness in less than one<br /> year; V1515 Cyg is the only known example to require a decade to rise<br /> to visual maximum. Note, however, that the historical light curves for many systems<br /> are poorly documented.<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|450px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|450px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1509 2013-07-26T10:54:15Z

<p>Chris.davis: /* T Tauri stars and other young variables and transients */</p> <hr /> <div>== T Tauri stars and other young variables and transients ==<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars (TTSs) are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; yr), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;), pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989]. They are optically visible (spectral type F,G,K,M) and their spectral energy distributions possess a modest excess in the near- and mid-IR, although the slope of their SED in the IR is still negative. Classical TTSs (Class II Young Stellar Objects) exhibit strong forbidden emission lines from ionised oxygen, sulphure, iron, etc., and they are often associated with Herbig-Haro jets; weak-lined TTSs (Class III YSOs) are essentially line-free. <br /> <br /> Class I YSOs possess a very strong IR excess (flat or positive spectral indices), are embedded, and are brighter in the near- and mid-IR bands. There is some statistical evidence that Class I YSOs - protostars - are the progenitors of TTSs; they are typically less abundant than Class II YSOs, are more likely to coincide with dark clouds and molecular cores, and may be much younger (&lt; 100,000 yr).<br /> <br /> T Tauri stars are known to vary on periods of days, weeks, and months. Causes include episodic accretion events, warped disk occultations, the transit of dark spots in the photosphere.<br /> <br /> Relevant characteristics of TTSs:<br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> Some young pre-main-sequence stars have exhibited quite drastic episodic variations. <br /> 1-3 mag eruptions have been observed in several objects (e.g. EX Lup, DR Tau), while<br /> more spectacular eruptions corresponding to a brightening of 3-6 mag have been measured<br /> in FU Orionis type variables (FU-ors). A dozen young stars are now characterised as FUors. Most have<br /> been observed to rise 3-5 mag in brightness in less than one<br /> year; V1515 Cyg is the only known example to require a decade to rise<br /> to visual maximum. Note, however, that the historical light curves for many systems<br /> are poorly documented.<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|450px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|450px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1508 2013-07-26T10:53:38Z

<p>Chris.davis: /* T Tauri stars and other young variables and transients */</p> <hr /> <div>== T Tauri stars and other young variables and transients ==<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars (TTSs) are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; yr), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;), pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989]. They are optically visible (spectral type F,G,K,M) and their spectral energy distributions possess a modest excess in the near- and mid-IR, although the slope of their SED in the IR is still negative. Classical TTSs (Class II Young Stellar Objects) exhibit strong forbidden emission lines from ionised oxygen, sulphure, iron, etc., and they are often associated with Herbig-Haro jets; weak-lined TTSs (Class III YSOs) are essentially line-free. <br /> <br /> Class I YSOs possess a very strong IR excess (flat or positive spectral indices), are embedded, and are brighter in the near- and mid-IR bands. There is some statistical evidence that Class I YSOs - protostars - are the progenitors of TTSs; they are typically less abundant than Class II YSOs, are more likely to coincide with dark clouds and molecular cores, and may be much younger (&lt; 100,000 yr).<br /> <br /> T Tauri stars are known to vary on periods of days, weeks, and months. Causes include episodic accretion events, warped disk occultations, the transit of dark spots in the photosphere.<br /> <br /> Relevant characteristics of TTSs:<br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> Some young pre-main-sequence stars have exhibited quite drastic episodic variations. <br /> 1-3 mag eruptions have been observed in several objects (e.g. EX Lup, DR Tau), while<br /> more spectacular eruptions corresponding to a brightening of 3-6 mag have been measured<br /> in FU Orionis type variables (FU-ors). A dozen young stars are now characterised as FUors. Most have<br /> been observed to rise 3-5 mag in brightness in less than one<br /> year; V1515 Cyg is the only known example to require a decade to rise<br /> to visual maximum. Note, however, that the historical light curves for many systems<br /> are poorly documented.<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|500px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|500px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1507 2013-07-26T10:52:49Z

<p>Chris.davis: /* T Tauri stars and other young variables and transients */</p> <hr /> <div>== T Tauri stars and other young variables and transients ==<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars (TTSs) are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; yr), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;), pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989]. They are optically visible (spectral type F,G,K,M) and their spectral energy distributions possess a modest excess in the near- and mid-IR, although the slope of their SED in the IR is still negative. Classical TTSs (Class II Young Stellar Objects) exhibit strong forbidden emission lines from ionised oxygen, sulphure, iron, etc., and they are often associated with Herbig-Haro jets; weak-lined TTSs (Class III YSOs) are essentially line-free. <br /> <br /> Class I YSOs possess a very strong IR excess (flat or positive spectral indices), are embedded, and are brighter in the near- and mid-IR bands. There is some statistical evidence that Class I YSOs - protostars - are the progenitors of TTSs; they are typically less abundant than Class II YSOs, are more likely to coincide with dark clouds and molecular cores, and may be much younger (&lt; 100,000 yr).<br /> <br /> T Tauri stars are known to vary on periods of days, weeks, and months. Causes include episodic accretion events, warped disk occultations, the transit of dark spots in the photosphere.<br /> <br /> Relevant characteristics of TTSs:<br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> Some young pre-main-sequence stars have exhibited quite drastic episodic variations. <br /> 1-3 mag eruptions have been observed in several objects (e.g. EX Lup, DR Tau), while<br /> more spectacular eruptions corresponding to a brightening of 3-6 mag have been measured<br /> in FU Orionis type variables (FU-ors). A dozen young stars are now characterised as FUors. Most have<br /> been observed to rise 3-5 mag in brightness in less than one<br /> year; V1515 Cyg is the only known example to require a decade to rise<br /> to visual maximum. Note, however, that the historical light curves for many systems<br /> are poorly documented.<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|400px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|400px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1506 2013-07-26T10:52:29Z

<p>Chris.davis: /* T Tauri stars and other young variables and transients */</p> <hr /> <div>== T Tauri stars and other young variables and transients ==<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars (TTSs) are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; y), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;), pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989]. They are optically visible (spectral type F,G,K,M) and their spectral energy distributions possess a modest excess in the near- and mid-IR, although the slope of their SED in the IR is still negative. Classical TTSs (Class II Young Stellar Objects) exhibit strong forbidden emission lines from ionised oxygen, sulphure, iron, etc., and they are often associated with Herbig-Haro jets; weak-lined TTSs (Class III YSOs) are essentially line-free. <br /> <br /> Class I YSOs possess a very strong IR excess (flat or positive spectral indices), are embedded, and are brighter in the near- and mid-IR bands. There is some statistical evidence that Class I YSOs - protostars - are the progenitors of TTSs; they are typically less abundant than Class II YSOs, are more likely to coincide with dark clouds and molecular cores, and may be much younger (&lt;math&gt; &lt;100,000 &lt;/math&gt; y).<br /> <br /> T Tauri stars are known to vary on periods of days, weeks, and months. Causes include episodic accretion events, warped disk occultations, the transit of dark spots in the photosphere.<br /> <br /> Relevant characteristics of TTSs:<br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> Some young pre-main-sequence stars have exhibited quite drastic episodic variations. <br /> 1-3 mag eruptions have been observed in several objects (e.g. EX Lup, DR Tau), while<br /> more spectacular eruptions corresponding to a brightening of 3-6 mag have been measured<br /> in FU Orionis type variables (FU-ors). A dozen young stars are now characterised as FUors. Most have<br /> been observed to rise 3-5 mag in brightness in less than one<br /> year; V1515 Cyg is the only known example to require a decade to rise<br /> to visual maximum. Note, however, that the historical light curves for many systems<br /> are poorly documented.<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|400px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|400px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1505 2013-07-26T10:51:03Z

<p>Chris.davis: /* T Tauri stars and other young variables and transients */</p> <hr /> <div>== T Tauri stars and other young variables and transients ==<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars (TTSs) are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; y), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;), pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989]. They are optically visible (spectral type F,G,K,M) and their spectral energy distributions possess a modest excess in the near- and mid-IR, although the slope of their SED in the IR is still negative. Classical TTSs (Class II Young Stellar Objects) exhibit strong forbidden emission lines from ionised oxygen, sulphure, iron, etc., and they are often associated with Herbig-Haro jets; weak-lined TTSs (Class III YSOs) are essentially line-free. <br /> <br /> Class I YSOs possess a very strong IR excess (flat or positive spectral indices), are embedded, and are brighter in the near- and mid-IR bands. There is some statistical evidence that Class I YSOs - protostars - are the progenitors of TTSs; they are typically less abundant than Class II YSOs, are more likely to coincide with dark clouds and molecular cores, and may be much younger (&lt;math&gt; &lt;10^5 &lt;/math&gt; y).<br /> <br /> T Tauri stars are known to vary on periods of days, weeks, and months. Causes include episodic accretion events, warped disk occultations, the transit of dark spots in the photosphere.<br /> <br /> Relevant characteristics of TTSs:<br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> Some young pre-main-sequence stars have exhibited quite drastic episodic variations. <br /> 1-3 mag eruptions have been observed in several objects (e.g. EX Lup, DR Tau), while<br /> more spectacular eruptions corresponding to a brightening of 3-6 mag have been measured<br /> in FU Orionis type variables (FU-ors). A dozen young stars are now characterised as FUors. Most have<br /> been observed to rise 3-5 mag in brightness in less than one<br /> year; V1515 Cyg is the only known example to require a decade to rise<br /> to visual maximum. Note, however, that the historical light curves for many systems<br /> are poorly documented.<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|400px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|400px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1504 2013-07-26T10:50:10Z

<p>Chris.davis: /* T Tauri stars and other young variables and transients */</p> <hr /> <div>== T Tauri stars and other young variables and transients ==<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars (TTSs) are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; y), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;), pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989]. They are optically visible (spectral type F,G,K,M) and their spectral energy distributions possess a modest excess in the near- and mid-IR, although the slope of their SED in the IR is still negative. Classical TTSs (Class II Young Stellar Objects) exhibit strong forbidden emission lines from ionised oxygen, sulphure, iron, etc., and they are often associated with Herbig-Haro jets; weak-lined TTSs (Class III YSOs) are essentially line-free. <br /> <br /> Class I YSOs possess a very strong IR excess (flat or positive spectral indices), are embedded, and are brighter in the near- and mid-IR bands. There is some statistical evidence that Class I YSOs - protostars - are the progenitors of TTSs; they are typically less abundant than Class II YSOs, are more likely to coincide with dark clouds and molecular cores, and may be much younger ( &lt;math&gt; &lt; 10^5 &lt;/math&gt; y).<br /> <br /> T Tauri stars are known to vary on periods of days, weeks, and months. Causes include episodic accretion events, warped disk occultations, the transit of dark spots in the photosphere.<br /> <br /> Relevant characteristics of TTSs:<br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> Some young pre-main-sequence stars have exhibited quite drastic episodic variations. <br /> 1-3 mag eruptions have been observed in several objects (e.g. EX Lup, DR Tau), while<br /> more spectacular eruptions corresponding to a brightening of 3-6 mag have been measured<br /> in FU Orionis type variables (FU-ors). A dozen young stars are now characterised as FUors. Most have<br /> been observed to rise 3-5 mag in brightness in less than one<br /> year; V1515 Cyg is the only known example to require a decade to rise<br /> to visual maximum. Note, however, that the historical light curves for many systems<br /> are poorly documented.<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|400px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|400px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1503 2013-07-26T10:47:08Z

<p>Chris.davis: /* T Tauri stars and other young variables and transients */</p> <hr /> <div>== T Tauri stars and other young variables and transients ==<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars (TTSs) are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; y), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;), pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989]. They are optically visible (spectral type F,G,K,M) and their spectral energy distributions possess a modest excess in the near- and mid-IR, although the slope of their SED in the IR is still negative. Classical TTSs (Class II Young Stellar Objects) exhibit strong forbidden emission lines from ionised oxygen, sulphure, iron, etc., and they are often associated with Herbig-Haro jets; weak-lined TTSs (Class III YSOs) are essentially line-free. <br /> <br /> Class I YSOs possess a very strong IR excess (flat or positive spectral indices), are embedded, and are brighter in the near- and mid-IR bands. There is some statistical evidence that Class I YSOs - protostars - are the progenitors of TTSs; they are typically less abundant than Class II YSOs, are more likely to coincide with dark clouds and molecular cores, and may be much younger ( &lt;math&gt; ~10^5 &lt;/math&gt; y).<br /> <br /> T Tauri stars are known to vary on periods of days, weeks, and months. Causes include episodic accretion events, warped disk occultations, the transit of dark spots in the photosphere.<br /> <br /> Relevant characteristics of TTSs:<br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> Some young pre-main-sequence stars have exhibited quite drastic episodic variations. <br /> 1-3 mag eruptions have been observed in several objects (e.g. EX Lup, DR Tau), while<br /> more spectacular eruptions corresponding to a brightening of 3-6 mag have been measured<br /> in FU Orionis type variables (FU-ors). A dozen young stars are now characterised as FUors. Most have<br /> been observed to rise 3-5 mag in brightness in less than one<br /> year; V1515 Cyg is the only known example to require a decade to rise<br /> to visual maximum. Note, however, that the historical light curves for many systems<br /> are poorly documented.<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|400px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|400px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1502 2013-07-26T10:31:38Z

<p>Chris.davis: /* T Tauri stars and other young variables and transients */</p> <hr /> <div>== T Tauri stars and other young variables and transients ==<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars (TTSs) are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; y), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;) pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989]. They are optically visible (spectral type F,G,K,M) and their spectral energy distributions possess a modest excess in the near- and mid-IR, although the slope of their SED in the IR is still negative. Classical TTSs (Class II Young Stellar Objects) exhibit strong forbidden emission lines from ionised oxygen, sulphure, iron, etc., and are often associated with Herbig-Haro jets. <br /> <br /> Characteristics:<br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> Some young pre-main-sequence stars have exhibited quite drastic episodic variations. FU Ori <br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|400px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|400px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1501 2013-07-26T10:21:52Z

<p>Chris.davis: /* T Tauri stars */</p> <hr /> <div>== T Tauri stars and other young variables and transients ==<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; y), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;) pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989].<br /> <br /> Characteristics:<br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|400px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|400px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]</div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=File:CTTS-spectra.jpeg&diff=1500 2013-07-26T10:20:25Z

<p>Chris.davis: </p> <hr /> <div></div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=File:FUori-spectra.jpeg&diff=1499 2013-07-26T10:19:47Z

<p>Chris.davis: </p> <hr /> <div></div>

Chris.davis https://gsawg.wiki.ast.cam.ac.uk/index.php?title=Triggers:TTau&diff=1498 2013-07-26T10:19:25Z

<p>Chris.davis: /* T Tauri stars */</p> <hr /> <div>== T Tauri stars ==<br /> [[File:figure_ttau_mag.png|400px|right|thumb|T Cha - example of TTau star from the ASAS data]]<br /> <br /> T Tauri type stars are very young (&lt;math&gt; &lt;10^7 &lt;/math&gt; y), low mass (&lt;math&gt; &lt;3 M^{}_\odot &lt;/math&gt;) pre-main sequence objects [http://adsabs.harvard.edu/abs/1989A%26ARv...1..291A Appenzeller &amp; Mundt 1989].<br /> <br /> Characteristics:<br /> * irregular and quasi-periodic variations<br /> * high amplitude (up to 5 mag)<br /> * may have a phase of quiescence (see figure)<br /> * absolute magnitude range: M_V=? to ? mag<br /> * typically do not require a trigger, but watch list of T Tauris would be useful<br /> <br /> Below are sample optical spectra of classical T Tauri stars and two FU-ori type eruptive variables.<br /> <br /> [[File:FUori-spectra.jpeg|400px|left|thumb|FRODOspec data from the Liverpool Telescope ]]<br /> [[File:CTTS-spectra.jpeg|400px|right|thumb|FRODOspec data of DG Tau (red), CW Tau (blue) and HL Tau (green) ]]</div>

Chris.davis