Gaia Science Alerts Working Group - User contributions [en]

File:Galaxies.jpg

2011-07-01T08:12:13Z

Gaia:

File:Nature09724-s1.pdf

2011-03-28T15:53:51Z

Gaia:

File:Nophoto.jpg

2011-03-28T15:37:36Z

Gaia:

Jctest2

2011-03-28T15:28:08Z

Gaia: Created page with 'Hello'

Hello

File:Uaf.pdf

2010-09-09T09:14:41Z

Gaia: For testing upload

For testing upload

Workshop2010:main

2010-03-15T13:09:44Z

Gaia:

== Welcome! ==

Gaia Science Alerts Workshop will take place in Cambridge on 23-25 June 2010.

* [[workshop2010:rationale|Rationale]]

* [[workshop2010:agenda|Agenda]]

* [[workshop2010:registration|Registration]]

* [[workshop2010:logistics|Logistic information]]

----
=== Workshop Organizing Committee ===

* Simon Hodgkin
* Lukasz Wyrzykowski

* Vasily Belokurov
* Wyn Evans
* Gerry Gilmore
* Floor van Leeuven
* Sergey Koposov
* Nick Walton

If you wish to contact the organizing committe, please email ''gsaw2010woc@ast.cam.ac.uk''.

----
=== Important Dates ===
* First announcement: '''1st March 2010'''
* Registration open: '''1st March 2010'''
* Registration closes: '''30 April 2010'''
* Support funding allocated: '''10 May 2010'''
* Invitations allocated: '''10 May 2010'''
* Accommodation and dinner payments: '''20 May 2010'''

Workshop2010:main

2010-03-15T13:01:10Z

Gaia:

== Welcome! ==

Gaia Science Alerts Workshop will take place in Cambridge on 23-25 June 2010.

* [[workshop2010:rationale|Rationale]]

* [[workshop2010:agenda|Agenda]]

* [[workshop2010:registration|Registration]]

* [[workshop2010:logistics|Logistic information]]

----
=== Workshop Organizing Committee ===

* Simon Hodgkin
* Lukasz Wyrzykowski

* Vasily Belokurov
* Wyn Evans
* Gerry Gilmore
* Floor van Leeuven
* Sergey Koposov
* Nick Walton
* Laurent Eyer

If you wish to contact the organizing committe, please email ''gsaw2010woc@ast.cam.ac.uk''.

----
=== Important Dates ===
* First announcement: '''1st March 2010'''
* Registration open: '''1st March 2010'''
* Registration closes: '''30 April 2010'''
* Support funding allocated: '''10 May 2010'''
* Invitations allocated: '''10 May 2010'''
* Accommodation and dinner payments: '''20 May 2010'''

Triggers:Supernovae

2009-08-10T14:35:45Z

Gaia: /* Supernova Types and Rates */

== Supernova Types and Rates ==

Numbers based on Belokurov and Evans (1993: MNRAS, 341, 569-576). Note that f in the table below is the fraction of all type-II supernovae that are L-type (they suggest using f=0.5).
The numbers are derived by taking the Galaxy number counts out to 75 Mpc and extrapolating as D^3. These are combined with supernova event rates compiled from the literature.

Although Belokuroav and Evans used an old scanning law to make their predictions, the numbers of total events down to G=20 will not change.

This magnitude limit corresponds to a distance of 630 Mpc for a type-Ia with an average G-band maximum magnitude of -18.99.

{| border="1" cellspacing=0 cellpadding="5" align="center"
! Type
! Total to G=20
|-
| Ia
| 48000
|-
| Ib
| 7000
|-
| IIL
| 28500*f
|-
| IIP
| 5600*(1-f)
|-
|}

The other piece of information needed is the Luminosity function. Supernova absolute magnitude distributions are also given in Belokurov and Evans. They
assume Gaussian distributions of absolute magnitude around maximum brightness as below:

{| border="1" cellspacing=0 cellpadding="5" align="center"
! Type
! <math>M_{G}</math>
! <math>\sigma_G</math>
|-
| 1a
| -18.99
| 0.76
|-
| 1b/c
| -17.75
| 1.29
|-
| II-L
| -17.63
| 0.88
|-
| II-P
| -16.44
| 1.23
|-
|}

== Supernovae type Ia ==

=== SDSS-II Supernova Survey (Stripe 82) ===
Stripe 82 spreads over 300 sq.deg between RA=-60 to RA=60 and Dec=-1.25 to Dec=+1.25.
It was monitored by SDSS in 5 filters (''ugriz'') since 1998, but more intensively in 2005 and 2006.
Numerous supernovae were found in 2005 season using difference imaging techniques, e.g. [http://ukads.nottingham.ac.uk/abs/2008AJ....135..348S Sako et al. 2008].

[[File:HoltzmanStripe82SNIa.jpg|600px]] From [http://ukads.nottingham.ac.uk/abs/2008AJ....136.2306H Holtzman et al. 2008].

== Supernovae type II ==

== Luminous Red Novae ==
The class of Luminous Red Novae was established in 2007 by Shrinivas Kulkarni classifying M85 OT2006-1 as LRN. It is disputed if it is a new class or subclass of SN-IIp.

* they are fainter than SNe and brighter than novae.
* they last over several weeks.
* distinctively red in colour, getting redder while fading

Triggers:Supernovae

2009-08-10T14:33:59Z

Gaia: /* Supernova Types and Rates */

== Supernova Types and Rates ==

Numbers based on Belokurov and Evans (1993: MNRAS, 341, 569-576). Note that f in the table below is the fraction of all type-II supernovae that are L-type (they suggest using f=0.5).
The numbers are derived by taking the Galaxy number counts out to 75 Mpc and extrapolating as D^3. These are combined with supernova event rates compiled from the literature.

Although Belokuroav and Evans used an old scanning law to make their predictions, the numbers of total events down to G=20 will not change.

This magnitude limit corresponds to a distance of 630 Mpc for a type-Ia with an average G-band maximum magnitude of -18.99.

{| border="1" cellspacing=0 cellpadding="5" align="center"
! Type
! Total to G=20
|-
| Ia
| 48000
|-
| Ib
| 7000
|-
| IIL
| 5600*f
|-
| IIP
| 28500*(1-f)
|-
|}

The other piece of information needed is the Luminosity function. Supernova absolute magnitude distributions are also given in Belokurov and Evans. They
assume Gaussian distributions of absolute magnitude around maximum brightness as below:

{| border="1" cellspacing=0 cellpadding="5" align="center"
! Type
! <math>M_{G}</math>
! <math>\sigma_G</math>
|-
| 1a
| -18.99
| 0.76
|-
| 1b/c
| -17.75
| 1.29
|-
| II-L
| -17.63
| 0.88
|-
| II-P
| -16.44
| 1.23
|-
|}

== Supernovae type Ia ==

=== SDSS-II Supernova Survey (Stripe 82) ===
Stripe 82 spreads over 300 sq.deg between RA=-60 to RA=60 and Dec=-1.25 to Dec=+1.25.
It was monitored by SDSS in 5 filters (''ugriz'') since 1998, but more intensively in 2005 and 2006.
Numerous supernovae were found in 2005 season using difference imaging techniques, e.g. [http://ukads.nottingham.ac.uk/abs/2008AJ....135..348S Sako et al. 2008].

[[File:HoltzmanStripe82SNIa.jpg|600px]] From [http://ukads.nottingham.ac.uk/abs/2008AJ....136.2306H Holtzman et al. 2008].

== Supernovae type II ==

== Luminous Red Novae ==
The class of Luminous Red Novae was established in 2007 by Shrinivas Kulkarni classifying M85 OT2006-1 as LRN. It is disputed if it is a new class or subclass of SN-IIp.

* they are fainter than SNe and brighter than novae.
* they last over several weeks.
* distinctively red in colour, getting redder while fading

Triggers:Supernovae

2009-08-10T14:30:51Z

Gaia: /* Supernova Types and Rates */

== Supernova Types and Rates ==

Numbers based on Belokurov and Evans (1993: MNRAS, 341, 569-576). Note that f in the table below is the fraction of all type-II supernovae that are L-type.
The numbers are derived by taking the Galaxy number counts out to 75 Mpc and extrapolating as D^3. These are combined with supernova event rates compiled from the literature.

Although Belokuroav and Evans used an old scanning law to make their predictions, the numbers of total events down to G=20 will not change.

This magnitude limit corresponds to a distance of 630 Mpc for a type-Ia with an average G-band maximum magnitude of -18.99.

{| border="1" cellspacing=0 cellpadding="5" align="center"
! Type
! Total to G=20
|-
| Ia
| 48000
|-
| Ib
| 7000
|-
| IIL
| 5600*f
|-
| IIP
| 28500*(1-f)
|-
|}

The other piece of information needed is the Luminosity function. Supernova absolute magnitude distributions are also given in Belokurov and Evans. They
assume Gaussian distributions of absolute magnitude around maximum brightness as below:

{| border="1" cellspacing=0 cellpadding="5" align="center"
! Type
! <math>M_{G}</math>
! <math>\sigma_G</math>
|-
| 1a
| -18.99
| 0.76
|-
| 1b/c
| -17.75
| 1.29
|-
| II-L
| -17.63
| 0.88
|-
| II-P
| -16.44
| 1.23
|-
|}

== Supernovae type Ia ==

=== SDSS-II Supernova Survey (Stripe 82) ===
Stripe 82 spreads over 300 sq.deg between RA=-60 to RA=60 and Dec=-1.25 to Dec=+1.25.
It was monitored by SDSS in 5 filters (''ugriz'') since 1998, but more intensively in 2005 and 2006.
Numerous supernovae were found in 2005 season using difference imaging techniques, e.g. [http://ukads.nottingham.ac.uk/abs/2008AJ....135..348S Sako et al. 2008].

[[File:HoltzmanStripe82SNIa.jpg|600px]] From [http://ukads.nottingham.ac.uk/abs/2008AJ....136.2306H Holtzman et al. 2008].

== Supernovae type II ==

== Luminous Red Novae ==
The class of Luminous Red Novae was established in 2007 by Shrinivas Kulkarni classifying M85 OT2006-1 as LRN. It is disputed if it is a new class or subclass of SN-IIp.

* they are fainter than SNe and brighter than novae.
* they last over several weeks.
* distinctively red in colour, getting redder while fading

Triggers:Supernovae

2009-08-10T14:30:02Z

Gaia: /* Supernova Types and Rates */

== Supernova Types and Rates ==

Numbers based on Belokurov and Evans (1993: MNRAS, 341, 569-576). Note that f in the table below is the fraction of all type-II supernovae that are L-type.
The numbers are derived by taking the Galaxy number counts out to 75 Mpc and extrapolating as D^3. These are combined with supernova event rates compiled from the literature.

Although Belokuroav and Evans used an old scanning law to make their predictions, the numbers of total events down to G=20 will not change.

This magnitude limit corresponds to a distance of 630 Mpc for a type-Ia with an average G-band maximum magnitude of -18.99.

{| border="1" cellspacing=0 cellpadding="5" align="center"
! Type
! Total to G=20
|-
| Ia
| 48000
|-
| Ib
| 7000
|-
| IIL
| 5600*f
|-
| IIP
| 28500*(1-f)
|-
|}

The other piece of information needed is the Luminosity function. Supernova absolute magnitude distributions are also given in Belokurov and Evans. They
assume Gaussian distributions of absolute magnitude around maximum brightness as below:

{| border="1" cellspacing=0 cellpadding="5" align="center"
! Type
! <math>M_{G}</math>
! <math>\sigma_G</match>
|-
| 1a
| -18.99
| 0.76
|-
| 1b/c
| -17.75
| 1.29
|-
| II-L
| -17.63
| 0.88
|-
| II-P
| -16.44
| 1.23
|-
|}

== Supernovae type Ia ==

=== SDSS-II Supernova Survey (Stripe 82) ===
Stripe 82 spreads over 300 sq.deg between RA=-60 to RA=60 and Dec=-1.25 to Dec=+1.25.
It was monitored by SDSS in 5 filters (''ugriz'') since 1998, but more intensively in 2005 and 2006.
Numerous supernovae were found in 2005 season using difference imaging techniques, e.g. [http://ukads.nottingham.ac.uk/abs/2008AJ....135..348S Sako et al. 2008].

[[File:HoltzmanStripe82SNIa.jpg|600px]] From [http://ukads.nottingham.ac.uk/abs/2008AJ....136.2306H Holtzman et al. 2008].

== Supernovae type II ==

== Luminous Red Novae ==
The class of Luminous Red Novae was established in 2007 by Shrinivas Kulkarni classifying M85 OT2006-1 as LRN. It is disputed if it is a new class or subclass of SN-IIp.

* they are fainter than SNe and brighter than novae.
* they last over several weeks.
* distinctively red in colour, getting redder while fading

Triggers:Supernovae

2009-08-10T14:27:17Z

Gaia: /* Supernova Types and Rates */

== Supernova Types and Rates ==

Numbers based on Belokurov and Evans (1993: MNRAS, 341, 569-576). Note that f in the table below is the fraction of all type-II supernovae that are L-type.
The numbers are derived by taking the Galaxy number counts out to 75 Mpc and extrapolating as D^3. These are combined with supernova event rates compiled from the literature.

Although Belokuroav and Evans used an old scanning law to make their predictions, the numbers of total events down to G=20 will not change.

This magnitude limit corresponds to a distance of 630 Mpc for a type-Ia with an average G-band maximum magnitude of -18.99.

{| border="1" cellspacing=0 cellpadding="5" align="center"
! Type
! Total to G=20
|-
| Ia
| 48000
|-
| Ib
| 7000
|-
| IIL
| 5600*f
|-
| IIP
| 28500*(1-f)
|-
|}

The other piece of information needed is the Luminosity function. Supernova absolute magnitude distributions are also given in Belokurov and Evans. They
assume Gaussian distributions of absolute magnitude around maximum brightness as below:

{| border="1" cellspacing=0 cellpadding="5" align="center"
! Type
! M\dG\u
! sigma\dG\u
|-
| 1a
| -18.99
| 0.76
|-
| 1b/c
| -17.75
| 1.29
|-
| II-L
| -17.63
| 0.88
|-
| II-P
| -16.44
| 1.23
|-
|}

== Supernovae type Ia ==

=== SDSS-II Supernova Survey (Stripe 82) ===
Stripe 82 spreads over 300 sq.deg between RA=-60 to RA=60 and Dec=-1.25 to Dec=+1.25.
It was monitored by SDSS in 5 filters (''ugriz'') since 1998, but more intensively in 2005 and 2006.
Numerous supernovae were found in 2005 season using difference imaging techniques, e.g. [http://ukads.nottingham.ac.uk/abs/2008AJ....135..348S Sako et al. 2008].

[[File:HoltzmanStripe82SNIa.jpg|600px]] From [http://ukads.nottingham.ac.uk/abs/2008AJ....136.2306H Holtzman et al. 2008].

== Supernovae type II ==

== Luminous Red Novae ==
The class of Luminous Red Novae was established in 2007 by Shrinivas Kulkarni classifying M85 OT2006-1 as LRN. It is disputed if it is a new class or subclass of SN-IIp.

* they are fainter than SNe and brighter than novae.
* they last over several weeks.
* distinctively red in colour, getting redder while fading

Triggers:Supernovae

2009-08-10T14:20:51Z

Gaia: /* Supernova Types and Rates */

== Supernova Types and Rates ==

Numbers based on Belokurov and Evans (1993: MNRAS, 341, 569-576). Note that f in the table below is the fraction of all type-II supernovae that are L-type.
The numbers are derived by taking the Galaxy number counts out to 75 Mpc and extrapolating as D^3. These are combined with supernova event rates compiled from the literature.

Although Belokuroav and Evans used an old scanning law to make their predictions, the numbers of total events down to G=20 will not change.

This magnitude limit corresponds to a distance of 630 Mpc for a type-Ia with an average G-band maximum magnitude of -18.99.

{| border="1" cellspacing=0 cellpadding="5" align="center"
! Type
! Total to G=20
|-
| Ia
| 48000
|-
| Ib
| 7000
|-
| IIL
| 5600*f
|-
| IIP
| 28500*(1-f)
|-
|}

The other piece of information needed is the Luminosity function

== Supernovae type Ia ==

=== SDSS-II Supernova Survey (Stripe 82) ===
Stripe 82 spreads over 300 sq.deg between RA=-60 to RA=60 and Dec=-1.25 to Dec=+1.25.
It was monitored by SDSS in 5 filters (''ugriz'') since 1998, but more intensively in 2005 and 2006.
Numerous supernovae were found in 2005 season using difference imaging techniques, e.g. [http://ukads.nottingham.ac.uk/abs/2008AJ....135..348S Sako et al. 2008].

[[File:HoltzmanStripe82SNIa.jpg|600px]] From [http://ukads.nottingham.ac.uk/abs/2008AJ....136.2306H Holtzman et al. 2008].

== Supernovae type II ==

== Luminous Red Novae ==
The class of Luminous Red Novae was established in 2007 by Shrinivas Kulkarni classifying M85 OT2006-1 as LRN. It is disputed if it is a new class or subclass of SN-IIp.

* they are fainter than SNe and brighter than novae.
* they last over several weeks.
* distinctively red in colour, getting redder while fading

Triggers:Supernovae

2009-08-10T14:12:05Z

Gaia: /* Supernovae type Ia */

== Supernova Types and Rates ==

Numbers based on Belokurov and Evans (1993: MNRAS, 341, 569-576)

{| border="1" cellspacing=0 cellpadding="5" align="center"
! Type
! Total to G=20
|-
| Ia
| 48000
|-
| Ib
| 7000
|-
| IIL
| 5600*f
|-
| IIP
| 28500*(1-f)
|-
|}

== Supernovae type Ia ==

=== SDSS-II Supernova Survey (Stripe 82) ===
Stripe 82 spreads over 300 sq.deg between RA=-60 to RA=60 and Dec=-1.25 to Dec=+1.25.
It was monitored by SDSS in 5 filters (''ugriz'') since 1998, but more intensively in 2005 and 2006.
Numerous supernovae were found in 2005 season using difference imaging techniques, e.g. [http://ukads.nottingham.ac.uk/abs/2008AJ....135..348S Sako et al. 2008].

[[File:HoltzmanStripe82SNIa.jpg|600px]] From [http://ukads.nottingham.ac.uk/abs/2008AJ....136.2306H Holtzman et al. 2008].

== Supernovae type II ==

== Luminous Red Novae ==
The class of Luminous Red Novae was established in 2007 by Shrinivas Kulkarni classifying M85 OT2006-1 as LRN. It is disputed if it is a new class or subclass of SN-IIp.

* they are fainter than SNe and brighter than novae.
* they last over several weeks.
* distinctively red in colour, getting redder while fading

Triggers:Supernovae

2009-08-10T14:03:44Z

Gaia: /* Supernovae type Ia */

== Supernova Types and Rates ==

Numbers based on Belokurov and Evans (1993: MNRAS, 341, 569-576)

{| border="1" cellspacing=0 cellpadding="5" align="center"
! Type
! Total to G=20
|-
| Ia
| 48000
|
|-
| Ib
| 7000
|
|-
| IIL
| 5600*f
|
|-
| IIP
| 28500*(1-f)
|
|-
|}

== Supernovae type Ia ==

=== SDSS-II Supernova Survey (Stripe 82) ===
Stripe 82 spreads over 300 sq.deg between RA=-60 to RA=60 and Dec=-1.25 to Dec=+1.25.
It was monitored by SDSS in 5 filters (''ugriz'') since 1998, but more intensively in 2005 and 2006.
Numerous supernovae were found in 2005 season using difference imaging techniques, e.g. [http://ukads.nottingham.ac.uk/abs/2008AJ....135..348S Sako et al. 2008].

[[File:HoltzmanStripe82SNIa.jpg|600px]] From [http://ukads.nottingham.ac.uk/abs/2008AJ....136.2306H Holtzman et al. 2008].

== Supernovae type II ==

== Luminous Red Novae ==
The class of Luminous Red Novae was established in 2007 by Shrinivas Kulkarni classifying M85 OT2006-1 as LRN. It is disputed if it is a new class or subclass of SN-IIp.

* they are fainter than SNe and brighter than novae.
* they last over several weeks.
* distinctively red in colour, getting redder while fading