Difference: VOSchool09 (1 vs. 13)

Revision 1303 Mar 2009 - Main.TWikiAdminUser

 

EuroVO-AIDA School 2009

Please go to this page

Changed:
<
<

Tools

>
>
This page will be deleted soon
Deleted:
<
<

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI
Participants

Dubinovska (Linux), Heraudeau (Max OS X), Marchetti (Linux), Nikolajuk (Linux), Olivares (Windows), Perez-Torres (Mac OS X), Suhada (Mac OS X), Toribio (Linux), Tremou (Linux), Tundo (Linux)

Group Web Page

Extragalactic 2

Tutors: Mark ALLEN, Eduardo GONZALEZ SOLARES
Participants

Baldi (Linux), Bonchi (Windows), Cassara' (Windows), Chon (Mac OS X), Finet (Windows/Linux), Fritz (Mac OS X), Guelbenzu (Linux), Leitet (Mac OS X), Messias (Mac OS X), Tepper-Garcia (Mac OS X), Vulcani (Mac OS X)

Group Web Page

Galactic 1

Tutors: Deborah BAINES, Nick WALTON

Participants

Belcheva (Linux), Borisova (Linux), Bragaglia (Mac OS X), Follert (Windows/Linux), Graefe (Linux), Nikolov (Linux), Raddi (Mac OS X), Stiele (Linux), Tempel (Mac OS X), Tuvikene (Windows)

Group Web Page

Galactic 2

Tutors: Caroline BOT, Enrique SOLANO, Sebastien DERRIERE

Participants

Alvarez-Iglesias (Linux), Hacar (Linux), Kovacevic (Windows), Oreiro (Linux), Sanchez-Ayaso (Linux), Santander-Vela (Mac OS X), Valdivielso (Linux/Windows), Vinatier (Windows/Linux), Zloczewski (Linux)

Group Web Page

-- EvanthiaHatziminaoglou - 24 Feb 2009

 

Revision 1203 Mar 2009 - Main.TWikiAdminUser

 

EuroVO-AIDA School 2009

Added:
>
>

Please go to this page

 

Tools

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI
Participants

Dubinovska (Linux), Heraudeau (Max OS X), Marchetti (Linux), Nikolajuk (Linux), Olivares (Windows), Perez-Torres (Mac OS X), Suhada (Mac OS X), Toribio (Linux), Tremou (Linux), Tundo (Linux)

Group Web Page

Extragalactic 2

Tutors: Mark ALLEN, Eduardo GONZALEZ SOLARES
Participants

Baldi (Linux), Bonchi (Windows), Cassara' (Windows), Chon (Mac OS X), Finet (Windows/Linux), Fritz (Mac OS X), Guelbenzu (Linux), Leitet (Mac OS X), Messias (Mac OS X), Tepper-Garcia (Mac OS X), Vulcani (Mac OS X)

Group Web Page

Galactic 1

Tutors: Deborah BAINES, Nick WALTON

Participants

Belcheva (Linux), Borisova (Linux), Bragaglia (Mac OS X), Follert (Windows/Linux), Graefe (Linux), Nikolov (Linux), Raddi (Mac OS X), Stiele (Linux), Tempel (Mac OS X), Tuvikene (Windows)

Group Web Page

Galactic 2

Tutors: Caroline BOT, Enrique SOLANO, Sebastien DERRIERE

Participants

Alvarez-Iglesias (Linux), Hacar (Linux), Kovacevic (Windows), Oreiro (Linux), Sanchez-Ayaso (Linux), Santander-Vela (Mac OS X), Valdivielso (Linux/Windows), Vinatier (Windows/Linux), Zloczewski (Linux)

Group Web Page

-- EvanthiaHatziminaoglou - 24 Feb 2009

Revision 1102 Mar 2009 - Main.PaoloPadovani

 

EuroVO-AIDA School 2009

Tools

Changed:
<
<
>
>
 

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI
Participants

Dubinovska (Linux), Heraudeau (Max OS X), Marchetti (Linux), Nikolajuk (Linux), Olivares (Windows), Perez-Torres (Mac OS X), Suhada (Mac OS X), Toribio (Linux), Tremou (Linux), Tundo (Linux)

Group Web Page

Extragalactic 2

Tutors: Mark ALLEN, Eduardo GONZALEZ SOLARES
Participants

Baldi (Linux), Bonchi (Windows), Cassara' (Windows), Chon (Mac OS X), Finet (Windows/Linux), Fritz (Mac OS X), Guelbenzu (Linux), Leitet (Mac OS X), Messias (Mac OS X), Tepper-Garcia (Mac OS X), Vulcani (Mac OS X)

Group Web Page

Galactic 1

Tutors: Deborah BAINES, Nick WALTON

Participants

Belcheva (Linux), Borisova (Linux), Bragaglia (Mac OS X), Follert (Windows/Linux), Graefe (Linux), Nikolov (Linux), Raddi (Mac OS X), Stiele (Linux), Tempel (Mac OS X), Tuvikene (Windows)

Group Web Page

Galactic 2

Tutors: Caroline BOT, Enrique SOLANO, Sebastien DERRIERE

Participants

Alvarez-Iglesias (Linux), Hacar (Linux), Kovacevic (Windows), Oreiro (Linux), Sanchez-Ayaso (Linux), Santander-Vela (Mac OS X), Valdivielso (Linux/Windows), Vinatier (Windows/Linux), Zloczewski (Linux)

Group Web Page

-- EvanthiaHatziminaoglou - 24 Feb 2009

Revision 1002 Mar 2009 - Main.EvanthiaHatziminaoglou

 

EuroVO-AIDA School 2009

Changed:
<
<
Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VOSA
  • (7) VirGO
>
>

Tools

Added:
>
>
 

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI
Participants
Changed:
<
<
Dubinovska (Linux), Heraudeau (Max OS X), Marchetti (Linux), Nikolajuk (Linux), Olivares (Windows), Perez Torres (Mac OS X), Suhada (Mac OS X), Toribio (Linux), Tremou (Linux), Tundo (Linux)
>
>
Dubinovska (Linux), Heraudeau (Max OS X), Marchetti (Linux), Nikolajuk (Linux), Olivares (Windows), Perez-Torres (Mac OS X), Suhada (Mac OS X), Toribio (Linux), Tremou (Linux), Tundo (Linux)
  Group Web Page

Extragalactic 2

Changed:
<
<
Tutors: Mark ALLEN, Eduardo GONZALEZ SOLARES, Giuseppe LONGO
>
>
Tutors: Mark ALLEN, Eduardo GONZALEZ SOLARES
 
Participants
Changed:
<
<
Baldi (Linux), Bonchi (Windows), Cassara' (Windows), Chon (Mac OS X), Finet (Windows/Linux), Fritz (Mac OS X), Guelbenzu (Linux), Leitet (Mac OS X), Messias (Mac OS X), Tepper Garcia (Mac OS X), Vulcani (Mac OS X)
>
>
Baldi (Linux), Bonchi (Windows), Cassara' (Windows), Chon (Mac OS X), Finet (Windows/Linux), Fritz (Mac OS X), Guelbenzu (Linux), Leitet (Mac OS X), Messias (Mac OS X), Tepper-Garcia (Mac OS X), Vulcani (Mac OS X)
  Group Web Page

Galactic 1

Tutors: Deborah BAINES, Nick WALTON

Participants
Changed:
<
<
Belcheva (Linux), Borisova (Linux), Bragaglia (Mac OS X), Follert (Windows/Linux), Graefe (Linux), Nikolov (Linux), Raddi (Mac OS X), Stiele (Linux), Tempel (Mac OS X, Tuvikene (Windows)
>
>
Belcheva (Linux), Borisova (Linux), Bragaglia (Mac OS X), Follert (Windows/Linux), Graefe (Linux), Nikolov (Linux), Raddi (Mac OS X), Stiele (Linux), Tempel (Mac OS X), Tuvikene (Windows)
  Group Web Page

Galactic 2

Tutors: Caroline BOT, Enrique SOLANO, Sebastien DERRIERE

Participants
Changed:
<
<
Alvarez Iglesias (Linux), Hacar (Linux), Kovacevic (Windows), Oreiro (Linux), Sanchez Ayaso (Linux), Santander Vela (Mac OS X), Valdivielso (Linux/Windows), Vinatier (Windows/Linux, Zloczewski (Linux)
>
>
Alvarez-Iglesias (Linux), Hacar (Linux), Kovacevic (Windows), Oreiro (Linux), Sanchez-Ayaso (Linux), Santander-Vela (Mac OS X), Valdivielso (Linux/Windows), Vinatier (Windows/Linux), Zloczewski (Linux)
  Group Web Page

-- EvanthiaHatziminaoglou - 24 Feb 2009

Revision 902 Mar 2009 - Main.PaoloPadovani

 

EuroVO-AIDA School 2009

Deleted:
<
<

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI
 
Deleted:
<
<
Search for ULX sources and X-ray binaries in nearby (D<10 Mpc) galaxies. Based on the case presented by M. Perez-Torres.

  • Start with 2XMM catalogue
  • Use different catalogues to search for X-ray counterparts of point-like sources
  • ??
Mining the ESO archive using VirGO ; import VOTables; send data to Aladin (images) and SPLAT (spectra);
 
Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
Changed:
<
<
  • (6) VirGO
>
>
  • (6) VOSA
Added:
>
>
  • (7) VirGO

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI
 
Participants
Changed:
<
<
Nikolajuk (Linux), Dubinovska (Linux), Suhada (Mac OS X), Tremou (Linux), Toribio (Linux), Tundo (Linux), Perez Torres (Mac OS X), Marchetti (Linux), Heraudeau (Max OS X), Olivares (Windows)
>
>
Dubinovska (Linux), Heraudeau (Max OS X), Marchetti (Linux), Nikolajuk (Linux), Olivares (Windows), Perez Torres (Mac OS X), Suhada (Mac OS X), Toribio (Linux), Tremou (Linux), Tundo (Linux)
Added:
>
>
Group Web Page
 

Extragalactic 2

Tutors: Mark ALLEN, Eduardo GONZALEZ SOLARES, Giuseppe LONGO
Added:
>
>
Participants
 
Changed:
<
<
Suggestion: Eduardo's case from the VO Info Day in Lisbon (http://www.sim.ul.pt/WorkshopVO-pt2008/prog/prog.html)
>
>
Baldi (Linux), Bonchi (Windows), Cassara' (Windows), Chon (Mac OS X), Finet (Windows/Linux), Fritz (Mac OS X), Guelbenzu (Linux), Leitet (Mac OS X), Messias (Mac OS X), Tepper Garcia (Mac OS X), Vulcani (Mac OS X)
 
Changed:
<
<
Comment by Enrique (02Mar): If I remember correctly part of the workflow can be easier done using VOSA. So I have added VOSA to the list of tools
>
>
Group Web Page
 
Deleted:
<
<
Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VOSA
 
Deleted:
<
<
Participants

Leitet (Mac OS X), Messias (Mac OS X), Finet (Windows/Linux), Tepper Garcia (Mac OS X), Baldi (Linux), Guelbenzu (Linux), Fritz (Mac OS X), Vulcani (Mac OS X), Cassara' (Windows), Chon (Mac OS X), Bonchi (Windows)
 

Galactic 1

Tutors: Deborah BAINES, Nick WALTON
Deleted:
<
<
Suggestion: use the IMF case developed by Evanthia, based on the VO-TECH Science Framework Document (see http://www.euro-vo.org/pub/fc/workflows/IMF.htm)
Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
 
Participants
Changed:
<
<
Belcheva (Linux), Bragaglia (Mac OS X), Tuvikene (Windows), Graefe (Linux), Follert (Windows/Linux), Raddi (Mac OS X), Nikolov (Linux), Borisova (Linux), Stiele (Linux), Tempel (Mac OS X)
>
>
Belcheva (Linux), Borisova (Linux), Bragaglia (Mac OS X), Follert (Windows/Linux), Graefe (Linux), Nikolov (Linux), Raddi (Mac OS X), Stiele (Linux), Tempel (Mac OS X, Tuvikene (Windows)
Added:
>
>
Group Web Page
 

Galactic 2

Tutors: Caroline BOT, Enrique SOLANO, Sebastien DERRIERE
Deleted:
<
<
Possible science case (from Alvarez Iglesias's case):

We propose to search for L and T candidate members in very young clusters (<10Myr) using data from UKIRT Deep Sky Survey (UKIDSS) and IRAC/Spitzer and a new method based on their Spectral Energy Distribution (SED) characterization.

The knowledge of the complete census of substellar objects in star forming regions with masses below the Deuterium burning limit (M=13 M_Jupiter, Saumon et al. 1996), nicknamed isolated planetary-mass objects (IPMOs) is very important to understand the formation processes of such low mass bodies. The origin of both IPMOs and PMOs around stars remains uncertain. It is likely that IPMOs form as a natural extension of the process that leads to the formation of low-mass stars and, probably, brown dwarfs, but they could also originate in proto-planetary discs and be ejected through dynamical interactions (e.g. Reipurth & Clarke 2001). One example of the usefulness of these searches is the deep photometric study by Caballero et al (2007) in the young (~3 Myr) and relatively close (~350 pc) Sigma Orionis cluster. In this case, they combined optical, near- and mid-IR data to characterize the sub-stellar population of the cluster down to ~ 5 M_J (~M6-L6) in an area of 790 arcmin^2. Their study indicates that both brown dwarfs and IPMOs could form as an extension of the low-mass star formation process.

An optical, near-infrared and mid-infrared photometric study on field M to T dwarfs is shown in Patten et al (2006). In this case, photometry from the Sloan Digital Sky Survey and IRAC/Spitzer was used to analyze the colors of 86 sources. They show that single colors are insufficient to determine univocally the spectral type. Spectral typing accuracy increases with the number of colors used in the analysis, which is virtually the same as having a well defined SED for each possible candidate. The J-H and H-K colors for T dwarfs become bluer with increasing spectral subtype, becoming degenerate with the colors of higher mass K and M dwarfs (Patten et al. 2006). IRAC/Spizer data are fundamental to break the degeneracy amongst different types shown in the near-IR. The four IRAC channels include the CH4 fundamental absorption at 3.3 microns, the continuum peak that is present for all objects cooler than 3000 K and the CO absorption at 4.7 microns, the H2O absorption in the 5.8 micron band and CH4 absorption in the 8 micron band.

We propose use the VO capabilities to perform a search for late M, L and T dwarf members in Orion based on the characterization of their SEDs. They will be constructed using data from UKIRT Deep Sky Survey (UKIDSS) and IRAC/Spitzer. We propose to compare the SED of all objects in the studied area with template observed SED’s of late L and T dwarfs using a least-squares minimization method similar to that proposed by the Bayo et al. 2008. They developed a tool (VOSA) within the VO to analyze and compare SEDs of sub-stellar objects with theoretical models. A similar study to Caballero et al. (2007) but in a more extended area could be done in the frame of the VO-AIDA 2009 School. The use of the SED-fitting method for detection of L and T’s using VO tools could be tested directly in the Sigma Orionis cluster, since despite the detailed work by Caballero et al., the full population of IPMOs is not known to its completeness. The method can also be tested on a different young cluster in Orion, like Epsilon Orionis or Delta Orionis. We expect that with the SED-minimization technique we can improve the detection efficiency of IPMOs in young clusters and find some new candidates that may remain uncovered from color-based searches. This scientific case will fully exploit the goals of the VO-AIDA 2009 School, since it will require amongst others the use of catalogue and table handling, image and spectra handling and least-squares minimization of large amounts of data. This project will need to make full use of ALADDIN, TOPCAT and VOSA amongst other VO tools. For the spectral-fitting step, we would ideally use VOSA to fit to template observed spectra, although good results can also be obtained by fitting to model spectra.

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VOSA ( Added by Enrique 02Mar)
 
Participants
Changed:
<
<
Alvarez Iglesias (Linux), Zloczewski (Linux), Valdivielso (Linux/Windows), Hacar (Linux), Sanchez Ayaso (Linux), Kovacevic (Windows), Oreiro (Linux), Santander Vela (Mac OS X), Vinatier (Windows/Linux)
>
>
Alvarez Iglesias (Linux), Hacar (Linux), Kovacevic (Windows), Oreiro (Linux), Sanchez Ayaso (Linux), Santander Vela (Mac OS X), Valdivielso (Linux/Windows), Vinatier (Windows/Linux, Zloczewski (Linux)
Added:
>
>
Group Web Page
  -- EvanthiaHatziminaoglou - 24 Feb 2009

Revision 802 Mar 2009 - Main.EvanthiaHatziminaoglou

 

EuroVO-AIDA School 2009

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI

Search for ULX sources and X-ray binaries in nearby (D<10 Mpc) galaxies. Based on the case presented by M. Perez-Torres.

  • Start with 2XMM catalogue
  • Use different catalogues to search for X-ray counterparts of point-like sources
  • ??
Mining the ESO archive using VirGO ; import VOTables; send data to Aladin (images) and SPLAT (spectra);

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VirGO
Participants
Changed:
<
<
Nikolajuk, Dubinovska, Suhada, Tremou, Toribio, Tundo, Perez Torres, Marchetti, Heraudeau, Olivares
>
>
Nikolajuk (Linux), Dubinovska (Linux), Suhada (Mac OS X), Tremou (Linux), Toribio (Linux), Tundo (Linux), Perez Torres (Mac OS X), Marchetti (Linux), Heraudeau (Max OS X), Olivares (Windows)
 

Extragalactic 2

Tutors: Mark ALLEN, Eduardo GONZALEZ SOLARES, Giuseppe LONGO

Suggestion: Eduardo's case from the VO Info Day in Lisbon (http://www.sim.ul.pt/WorkshopVO-pt2008/prog/prog.html)

Comment by Enrique (02Mar): If I remember correctly part of the workflow can be easier done using VOSA. So I have added VOSA to the list of tools

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VOSA

Participants
Changed:
<
<

Leitet, Messias, Finet, Tepper Garcia, Baldi, Guelbenzu, Fritz, Vulcani, Cassara', Chon, Bonchi
>
>

Leitet (Mac OS X), Messias (Mac OS X), Finet (Windows/Linux), Tepper Garcia (Mac OS X), Baldi (Linux), Guelbenzu (Linux), Fritz (Mac OS X), Vulcani (Mac OS X), Cassara' (Windows), Chon (Mac OS X), Bonchi (Windows)
 

Galactic 1

Tutors: Deborah BAINES, Nick WALTON

Suggestion: use the IMF case developed by Evanthia, based on the VO-TECH Science Framework Document (see http://www.euro-vo.org/pub/fc/workflows/IMF.htm)

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
Participants
Changed:
<
<
Belcheva, Bragaglia, Tuvikene, Graefe, Follert, Raddi, Nikolov, Borisova, Stiele, Tempel
>
>
Belcheva (Linux), Bragaglia (Mac OS X), Tuvikene (Windows), Graefe (Linux), Follert (Windows/Linux), Raddi (Mac OS X), Nikolov (Linux), Borisova (Linux), Stiele (Linux), Tempel (Mac OS X)
 

Galactic 2

Tutors: Caroline BOT, Enrique SOLANO, Sebastien DERRIERE

Possible science case (from Alvarez Iglesias's case):

We propose to search for L and T candidate members in very young clusters (<10Myr) using data from UKIRT Deep Sky Survey (UKIDSS) and IRAC/Spitzer and a new method based on their Spectral Energy Distribution (SED) characterization.

The knowledge of the complete census of substellar objects in star forming regions with masses below the Deuterium burning limit (M=13 M_Jupiter, Saumon et al. 1996), nicknamed isolated planetary-mass objects (IPMOs) is very important to understand the formation processes of such low mass bodies. The origin of both IPMOs and PMOs around stars remains uncertain. It is likely that IPMOs form as a natural extension of the process that leads to the formation of low-mass stars and, probably, brown dwarfs, but they could also originate in proto-planetary discs and be ejected through dynamical interactions (e.g. Reipurth & Clarke 2001). One example of the usefulness of these searches is the deep photometric study by Caballero et al (2007) in the young (~3 Myr) and relatively close (~350 pc) Sigma Orionis cluster. In this case, they combined optical, near- and mid-IR data to characterize the sub-stellar population of the cluster down to ~ 5 M_J (~M6-L6) in an area of 790 arcmin^2. Their study indicates that both brown dwarfs and IPMOs could form as an extension of the low-mass star formation process.

An optical, near-infrared and mid-infrared photometric study on field M to T dwarfs is shown in Patten et al (2006). In this case, photometry from the Sloan Digital Sky Survey and IRAC/Spitzer was used to analyze the colors of 86 sources. They show that single colors are insufficient to determine univocally the spectral type. Spectral typing accuracy increases with the number of colors used in the analysis, which is virtually the same as having a well defined SED for each possible candidate. The J-H and H-K colors for T dwarfs become bluer with increasing spectral subtype, becoming degenerate with the colors of higher mass K and M dwarfs (Patten et al. 2006). IRAC/Spizer data are fundamental to break the degeneracy amongst different types shown in the near-IR. The four IRAC channels include the CH4 fundamental absorption at 3.3 microns, the continuum peak that is present for all objects cooler than 3000 K and the CO absorption at 4.7 microns, the H2O absorption in the 5.8 micron band and CH4 absorption in the 8 micron band.

We propose use the VO capabilities to perform a search for late M, L and T dwarf members in Orion based on the characterization of their SEDs. They will be constructed using data from UKIRT Deep Sky Survey (UKIDSS) and IRAC/Spitzer. We propose to compare the SED of all objects in the studied area with template observed SED’s of late L and T dwarfs using a least-squares minimization method similar to that proposed by the Bayo et al. 2008. They developed a tool (VOSA) within the VO to analyze and compare SEDs of sub-stellar objects with theoretical models. A similar study to Caballero et al. (2007) but in a more extended area could be done in the frame of the VO-AIDA 2009 School. The use of the SED-fitting method for detection of L and T’s using VO tools could be tested directly in the Sigma Orionis cluster, since despite the detailed work by Caballero et al., the full population of IPMOs is not known to its completeness. The method can also be tested on a different young cluster in Orion, like Epsilon Orionis or Delta Orionis. We expect that with the SED-minimization technique we can improve the detection efficiency of IPMOs in young clusters and find some new candidates that may remain uncovered from color-based searches. This scientific case will fully exploit the goals of the VO-AIDA 2009 School, since it will require amongst others the use of catalogue and table handling, image and spectra handling and least-squares minimization of large amounts of data. This project will need to make full use of ALADDIN, TOPCAT and VOSA amongst other VO tools. For the spectral-fitting step, we would ideally use VOSA to fit to template observed spectra, although good results can also be obtained by fitting to model spectra.

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VOSA ( Added by Enrique 02Mar)

Participants
Changed:
<
<
Alvarez Iglesias, Zloczewski, Valdivielso, Hacar, Sanchez Ayaso, Kovacevic, Oreiro, Santander Vela, Vinatier
>
>
Alvarez Iglesias (Linux), Zloczewski (Linux), Valdivielso (Linux/Windows), Hacar (Linux), Sanchez Ayaso (Linux), Kovacevic (Windows), Oreiro (Linux), Santander Vela (Mac OS X), Vinatier (Windows/Linux)
  -- EvanthiaHatziminaoglou - 24 Feb 2009

Revision 702 Mar 2009 - Main.PaoloPadovani

 

EuroVO-AIDA School 2009

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI

Search for ULX sources and X-ray binaries in nearby (D<10 Mpc) galaxies. Based on the case presented by M. Perez-Torres.

  • Start with 2XMM catalogue
  • Use different catalogues to search for X-ray counterparts of point-like sources
  • ??
Changed:
<
<
Mining the ESO archive using VirGO ; import VOTables; send data to Aladin (images) and SPLAT (spectra);
>
>
Mining the ESO archive using VirGO ; import VOTables; send data to Aladin (images) and SPLAT (spectra);
 
Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VirGO
Participants

Nikolajuk, Dubinovska, Suhada, Tremou, Toribio, Tundo, Perez Torres, Marchetti, Heraudeau, Olivares

Extragalactic 2

Tutors: Mark ALLEN, Eduardo GONZALEZ SOLARES, Giuseppe LONGO

Suggestion: Eduardo's case from the VO Info Day in Lisbon (http://www.sim.ul.pt/WorkshopVO-pt2008/prog/prog.html)

Comment by Enrique (02Mar): If I remember correctly part of the workflow can be easier done using VOSA. So I have added VOSA to the list of tools

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VOSA

Participants

Leitet, Messias, Finet, Tepper Garcia, Baldi, Guelbenzu, Fritz, Vulcani, Cassara', Chon, Bonchi

Galactic 1

Tutors: Deborah BAINES, Nick WALTON

Suggestion: use the IMF case developed by Evanthia, based on the VO-TECH Science Framework Document (see http://www.euro-vo.org/pub/fc/workflows/IMF.htm)

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
Participants

Belcheva, Bragaglia, Tuvikene, Graefe, Follert, Raddi, Nikolov, Borisova, Stiele, Tempel

Galactic 2

Tutors: Caroline BOT, Enrique SOLANO, Sebastien DERRIERE

Possible science case (from Alvarez Iglesias's case):

We propose to search for L and T candidate members in very young clusters (<10Myr) using data from UKIRT Deep Sky Survey (UKIDSS) and IRAC/Spitzer and a new method based on their Spectral Energy Distribution (SED) characterization.

The knowledge of the complete census of substellar objects in star forming regions with masses below the Deuterium burning limit (M=13 M_Jupiter, Saumon et al. 1996), nicknamed isolated planetary-mass objects (IPMOs) is very important to understand the formation processes of such low mass bodies. The origin of both IPMOs and PMOs around stars remains uncertain. It is likely that IPMOs form as a natural extension of the process that leads to the formation of low-mass stars and, probably, brown dwarfs, but they could also originate in proto-planetary discs and be ejected through dynamical interactions (e.g. Reipurth & Clarke 2001). One example of the usefulness of these searches is the deep photometric study by Caballero et al (2007) in the young (~3 Myr) and relatively close (~350 pc) Sigma Orionis cluster. In this case, they combined optical, near- and mid-IR data to characterize the sub-stellar population of the cluster down to ~ 5 M_J (~M6-L6) in an area of 790 arcmin^2. Their study indicates that both brown dwarfs and IPMOs could form as an extension of the low-mass star formation process.

An optical, near-infrared and mid-infrared photometric study on field M to T dwarfs is shown in Patten et al (2006). In this case, photometry from the Sloan Digital Sky Survey and IRAC/Spitzer was used to analyze the colors of 86 sources. They show that single colors are insufficient to determine univocally the spectral type. Spectral typing accuracy increases with the number of colors used in the analysis, which is virtually the same as having a well defined SED for each possible candidate. The J-H and H-K colors for T dwarfs become bluer with increasing spectral subtype, becoming degenerate with the colors of higher mass K and M dwarfs (Patten et al. 2006). IRAC/Spizer data are fundamental to break the degeneracy amongst different types shown in the near-IR. The four IRAC channels include the CH4 fundamental absorption at 3.3 microns, the continuum peak that is present for all objects cooler than 3000 K and the CO absorption at 4.7 microns, the H2O absorption in the 5.8 micron band and CH4 absorption in the 8 micron band.

We propose use the VO capabilities to perform a search for late M, L and T dwarf members in Orion based on the characterization of their SEDs. They will be constructed using data from UKIRT Deep Sky Survey (UKIDSS) and IRAC/Spitzer. We propose to compare the SED of all objects in the studied area with template observed SED’s of late L and T dwarfs using a least-squares minimization method similar to that proposed by the Bayo et al. 2008. They developed a tool (VOSA) within the VO to analyze and compare SEDs of sub-stellar objects with theoretical models. A similar study to Caballero et al. (2007) but in a more extended area could be done in the frame of the VO-AIDA 2009 School. The use of the SED-fitting method for detection of L and T’s using VO tools could be tested directly in the Sigma Orionis cluster, since despite the detailed work by Caballero et al., the full population of IPMOs is not known to its completeness. The method can also be tested on a different young cluster in Orion, like Epsilon Orionis or Delta Orionis. We expect that with the SED-minimization technique we can improve the detection efficiency of IPMOs in young clusters and find some new candidates that may remain uncovered from color-based searches. This scientific case will fully exploit the goals of the VO-AIDA 2009 School, since it will require amongst others the use of catalogue and table handling, image and spectra handling and least-squares minimization of large amounts of data. This project will need to make full use of ALADDIN, TOPCAT and VOSA amongst other VO tools. For the spectral-fitting step, we would ideally use VOSA to fit to template observed spectra, although good results can also be obtained by fitting to model spectra.

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VOSA ( Added by Enrique 02Mar)

Participants

Alvarez Iglesias, Zloczewski, Valdivielso, Hacar, Sanchez Ayaso, Kovacevic, Oreiro, Santander Vela, Vinatier

-- EvanthiaHatziminaoglou - 24 Feb 2009

Revision 602 Mar 2009 - Main.EvanthiaHatziminaoglou

 

EuroVO-AIDA School 2009

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI
Changed:
<
<
Suggestion by Enrique (02Mar): The case proposed by Perez-Torres could be adequate. It is doable and uses several Aladin capabilities (e.g. filtering and cross-match).
>
>
Search for ULX sources and X-ray binaries in nearby (D<10 Mpc) galaxies. Based on the case presented by M. Perez-Torres.
Added:
>
>
  • Start with 2XMM catalogue
  • Use different catalogues to search for X-ray counterparts of point-like sources
  • ??
Mining the ESO archive using VirGO ; import VOTables; send data to Aladin (images) and SPLAT (spectra);
 
Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VirGO
Participants

Nikolajuk, Dubinovska, Suhada, Tremou, Toribio, Tundo, Perez Torres, Marchetti, Heraudeau, Olivares

Extragalactic 2

Tutors: Mark ALLEN, Eduardo GONZALEZ SOLARES, Giuseppe LONGO

Suggestion: Eduardo's case from the VO Info Day in Lisbon (http://www.sim.ul.pt/WorkshopVO-pt2008/prog/prog.html)

Comment by Enrique (02Mar): If I remember correctly part of the workflow can be easier done using VOSA. So I have added VOSA to the list of tools

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VOSA

Participants

Leitet, Messias, Finet, Tepper Garcia, Baldi, Guelbenzu, Fritz, Vulcani, Cassara', Chon, Bonchi

Galactic 1

Tutors: Deborah BAINES, Nick WALTON

Suggestion: use the IMF case developed by Evanthia, based on the VO-TECH Science Framework Document (see http://www.euro-vo.org/pub/fc/workflows/IMF.htm)

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
Participants

Belcheva, Bragaglia, Tuvikene, Graefe, Follert, Raddi, Nikolov, Borisova, Stiele, Tempel

Galactic 2

Tutors: Caroline BOT, Enrique SOLANO, Sebastien DERRIERE

Possible science case (from Alvarez Iglesias's case):

We propose to search for L and T candidate members in very young clusters (<10Myr) using data from UKIRT Deep Sky Survey (UKIDSS) and IRAC/Spitzer and a new method based on their Spectral Energy Distribution (SED) characterization.

The knowledge of the complete census of substellar objects in star forming regions with masses below the Deuterium burning limit (M=13 M_Jupiter, Saumon et al. 1996), nicknamed isolated planetary-mass objects (IPMOs) is very important to understand the formation processes of such low mass bodies. The origin of both IPMOs and PMOs around stars remains uncertain. It is likely that IPMOs form as a natural extension of the process that leads to the formation of low-mass stars and, probably, brown dwarfs, but they could also originate in proto-planetary discs and be ejected through dynamical interactions (e.g. Reipurth & Clarke 2001). One example of the usefulness of these searches is the deep photometric study by Caballero et al (2007) in the young (~3 Myr) and relatively close (~350 pc) Sigma Orionis cluster. In this case, they combined optical, near- and mid-IR data to characterize the sub-stellar population of the cluster down to ~ 5 M_J (~M6-L6) in an area of 790 arcmin^2. Their study indicates that both brown dwarfs and IPMOs could form as an extension of the low-mass star formation process.

An optical, near-infrared and mid-infrared photometric study on field M to T dwarfs is shown in Patten et al (2006). In this case, photometry from the Sloan Digital Sky Survey and IRAC/Spitzer was used to analyze the colors of 86 sources. They show that single colors are insufficient to determine univocally the spectral type. Spectral typing accuracy increases with the number of colors used in the analysis, which is virtually the same as having a well defined SED for each possible candidate. The J-H and H-K colors for T dwarfs become bluer with increasing spectral subtype, becoming degenerate with the colors of higher mass K and M dwarfs (Patten et al. 2006). IRAC/Spizer data are fundamental to break the degeneracy amongst different types shown in the near-IR. The four IRAC channels include the CH4 fundamental absorption at 3.3 microns, the continuum peak that is present for all objects cooler than 3000 K and the CO absorption at 4.7 microns, the H2O absorption in the 5.8 micron band and CH4 absorption in the 8 micron band.

We propose use the VO capabilities to perform a search for late M, L and T dwarf members in Orion based on the characterization of their SEDs. They will be constructed using data from UKIRT Deep Sky Survey (UKIDSS) and IRAC/Spitzer. We propose to compare the SED of all objects in the studied area with template observed SED’s of late L and T dwarfs using a least-squares minimization method similar to that proposed by the Bayo et al. 2008. They developed a tool (VOSA) within the VO to analyze and compare SEDs of sub-stellar objects with theoretical models. A similar study to Caballero et al. (2007) but in a more extended area could be done in the frame of the VO-AIDA 2009 School. The use of the SED-fitting method for detection of L and T’s using VO tools could be tested directly in the Sigma Orionis cluster, since despite the detailed work by Caballero et al., the full population of IPMOs is not known to its completeness. The method can also be tested on a different young cluster in Orion, like Epsilon Orionis or Delta Orionis. We expect that with the SED-minimization technique we can improve the detection efficiency of IPMOs in young clusters and find some new candidates that may remain uncovered from color-based searches. This scientific case will fully exploit the goals of the VO-AIDA 2009 School, since it will require amongst others the use of catalogue and table handling, image and spectra handling and least-squares minimization of large amounts of data. This project will need to make full use of ALADDIN, TOPCAT and VOSA amongst other VO tools. For the spectral-fitting step, we would ideally use VOSA to fit to template observed spectra, although good results can also be obtained by fitting to model spectra.

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VOSA ( Added by Enrique 02Mar)

Participants

Alvarez Iglesias, Zloczewski, Valdivielso, Hacar, Sanchez Ayaso, Kovacevic, Oreiro, Santander Vela, Vinatier

-- EvanthiaHatziminaoglou - 24 Feb 2009

Revision 502 Mar 2009 - Main.EvanthiaHatziminaoglou

 

EuroVO-AIDA School 2009

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI
Changed:
<
<
Suggestion by Enrique (02Mar): The case proposed by Perez-Torres could be adequate. It is doable and uses several Aladin capabilities (e.g. filtering and cross-match).
>
>
Suggestion by Enrique (02Mar): The case proposed by Perez-Torres could be adequate. It is doable and uses several Aladin capabilities (e.g. filtering and cross-match).
 
Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VirGO
Participants
Changed:
<
<
D'Odorico, Nikolajuk, Dubinovska, Suhada, Tremou, Toribio, Tundo, Perez Torres, Marchetti, De Boni, Heraudeau
>
>
Nikolajuk, Dubinovska, Suhada, Tremou, Toribio, Tundo, Perez Torres, Marchetti, Heraudeau, Olivares
 

Extragalactic 2

Tutors: Mark ALLEN, Eduardo GONZALEZ SOLARES, Giuseppe LONGO

Suggestion: Eduardo's case from the VO Info Day in Lisbon (http://www.sim.ul.pt/WorkshopVO-pt2008/prog/prog.html)

Comment by Enrique (02Mar): If I remember correctly part of the workflow can be easier done using VOSA. So I have added VOSA to the list of tools

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VOSA

Participants

Leitet, Messias, Finet, Tepper Garcia, Baldi, Guelbenzu, Fritz, Vulcani, Cassara', Chon, Bonchi

Galactic 1

Tutors: Deborah BAINES, Nick WALTON

Suggestion: use the IMF case developed by Evanthia, based on the VO-TECH Science Framework Document (see http://www.euro-vo.org/pub/fc/workflows/IMF.htm)

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
Participants
Changed:
<
<
Belcheva, Tuvikene, Eisenbeiss, Graefe, Follert, Raddi, Nikolov, Borisova, Stiele, Tempel
>
>
Belcheva, Bragaglia, Tuvikene, Graefe, Follert, Raddi, Nikolov, Borisova, Stiele, Tempel
 

Galactic 2

Tutors: Caroline BOT, Enrique SOLANO, Sebastien DERRIERE

Possible science case (from Alvarez Iglesias's case):

We propose to search for L and T candidate members in very young clusters (<10Myr) using data from UKIRT Deep Sky Survey (UKIDSS) and IRAC/Spitzer and a new method based on their Spectral Energy Distribution (SED) characterization.

The knowledge of the complete census of substellar objects in star forming regions with masses below the Deuterium burning limit (M=13 M_Jupiter, Saumon et al. 1996), nicknamed isolated planetary-mass objects (IPMOs) is very important to understand the formation processes of such low mass bodies. The origin of both IPMOs and PMOs around stars remains uncertain. It is likely that IPMOs form as a natural extension of the process that leads to the formation of low-mass stars and, probably, brown dwarfs, but they could also originate in proto-planetary discs and be ejected through dynamical interactions (e.g. Reipurth & Clarke 2001). One example of the usefulness of these searches is the deep photometric study by Caballero et al (2007) in the young (~3 Myr) and relatively close (~350 pc) Sigma Orionis cluster. In this case, they combined optical, near- and mid-IR data to characterize the sub-stellar population of the cluster down to ~ 5 M_J (~M6-L6) in an area of 790 arcmin^2. Their study indicates that both brown dwarfs and IPMOs could form as an extension of the low-mass star formation process.

An optical, near-infrared and mid-infrared photometric study on field M to T dwarfs is shown in Patten et al (2006). In this case, photometry from the Sloan Digital Sky Survey and IRAC/Spitzer was used to analyze the colors of 86 sources. They show that single colors are insufficient to determine univocally the spectral type. Spectral typing accuracy increases with the number of colors used in the analysis, which is virtually the same as having a well defined SED for each possible candidate. The J-H and H-K colors for T dwarfs become bluer with increasing spectral subtype, becoming degenerate with the colors of higher mass K and M dwarfs (Patten et al. 2006). IRAC/Spizer data are fundamental to break the degeneracy amongst different types shown in the near-IR. The four IRAC channels include the CH4 fundamental absorption at 3.3 microns, the continuum peak that is present for all objects cooler than 3000 K and the CO absorption at 4.7 microns, the H2O absorption in the 5.8 micron band and CH4 absorption in the 8 micron band.

We propose use the VO capabilities to perform a search for late M, L and T dwarf members in Orion based on the characterization of their SEDs. They will be constructed using data from UKIRT Deep Sky Survey (UKIDSS) and IRAC/Spitzer. We propose to compare the SED of all objects in the studied area with template observed SED’s of late L and T dwarfs using a least-squares minimization method similar to that proposed by the Bayo et al. 2008. They developed a tool (VOSA) within the VO to analyze and compare SEDs of sub-stellar objects with theoretical models. A similar study to Caballero et al. (2007) but in a more extended area could be done in the frame of the VO-AIDA 2009 School. The use of the SED-fitting method for detection of L and T’s using VO tools could be tested directly in the Sigma Orionis cluster, since despite the detailed work by Caballero et al., the full population of IPMOs is not known to its completeness. The method can also be tested on a different young cluster in Orion, like Epsilon Orionis or Delta Orionis. We expect that with the SED-minimization technique we can improve the detection efficiency of IPMOs in young clusters and find some new candidates that may remain uncovered from color-based searches. This scientific case will fully exploit the goals of the VO-AIDA 2009 School, since it will require amongst others the use of catalogue and table handling, image and spectra handling and least-squares minimization of large amounts of data. This project will need to make full use of ALADDIN, TOPCAT and VOSA amongst other VO tools. For the spectral-fitting step, we would ideally use VOSA to fit to template observed spectra, although good results can also be obtained by fitting to model spectra.

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
Changed:
<
<
  • (6) VOSA (Added by Enrique 02Mar)
>
>
  • (6) VOSA ( Added by Enrique 02Mar)
 

Participants
Changed:
<
<
Alvarez Iglesias, Zloczewski, Valdivielso, Hacar, Sanchez Ayaso, Kovacevic, Oreiro, Santander Vela
>
>
Alvarez Iglesias, Zloczewski, Valdivielso, Hacar, Sanchez Ayaso, Kovacevic, Oreiro, Santander Vela, Vinatier
  -- EvanthiaHatziminaoglou - 24 Feb 2009

Revision 402 Mar 2009 - Main.EnriqueSolano

 

EuroVO-AIDA School 2009

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI
Changed:
<
<
Title blabla
>
>
Suggestion by Enrique (02Mar): The case proposed by Perez-Torres could be adequate. It is doable and uses several Aladin capabilities (e.g. filtering and cross-match).
 
Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VirGO
Participants

D'Odorico, Nikolajuk, Dubinovska, Suhada, Tremou, Toribio, Tundo, Perez Torres, Marchetti, De Boni, Heraudeau

Extragalactic 2

Tutors: Mark ALLEN, Eduardo GONZALEZ SOLARES, Giuseppe LONGO

Suggestion: Eduardo's case from the VO Info Day in Lisbon (http://www.sim.ul.pt/WorkshopVO-pt2008/prog/prog.html)

Added:
>
>
Comment by Enrique (02Mar): If I remember correctly part of the workflow can be easier done using VOSA. So I have added VOSA to the list of tools
 
Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
Added:
>
>
  • (6) VOSA
 

Participants

Leitet, Messias, Finet, Tepper Garcia, Baldi, Guelbenzu, Fritz, Vulcani, Cassara', Chon, Bonchi

Galactic 1

Tutors: Deborah BAINES, Nick WALTON

Suggestion: use the IMF case developed by Evanthia, based on the VO-TECH Science Framework Document (see http://www.euro-vo.org/pub/fc/workflows/IMF.htm)

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
Participants

Belcheva, Tuvikene, Eisenbeiss, Graefe, Follert, Raddi, Nikolov, Borisova, Stiele, Tempel

Galactic 2

Tutors: Caroline BOT, Enrique SOLANO, Sebastien DERRIERE

Possible science case (from Alvarez Iglesias's case):

We propose to search for L and T candidate members in very young clusters (<10Myr) using data from UKIRT Deep Sky Survey (UKIDSS) and IRAC/Spitzer and a new method based on their Spectral Energy Distribution (SED) characterization.

The knowledge of the complete census of substellar objects in star forming regions with masses below the Deuterium burning limit (M=13 M_Jupiter, Saumon et al. 1996), nicknamed isolated planetary-mass objects (IPMOs) is very important to understand the formation processes of such low mass bodies. The origin of both IPMOs and PMOs around stars remains uncertain. It is likely that IPMOs form as a natural extension of the process that leads to the formation of low-mass stars and, probably, brown dwarfs, but they could also originate in proto-planetary discs and be ejected through dynamical interactions (e.g. Reipurth & Clarke 2001). One example of the usefulness of these searches is the deep photometric study by Caballero et al (2007) in the young (~3 Myr) and relatively close (~350 pc) Sigma Orionis cluster. In this case, they combined optical, near- and mid-IR data to characterize the sub-stellar population of the cluster down to ~ 5 M_J (~M6-L6) in an area of 790 arcmin^2. Their study indicates that both brown dwarfs and IPMOs could form as an extension of the low-mass star formation process.

An optical, near-infrared and mid-infrared photometric study on field M to T dwarfs is shown in Patten et al (2006). In this case, photometry from the Sloan Digital Sky Survey and IRAC/Spitzer was used to analyze the colors of 86 sources. They show that single colors are insufficient to determine univocally the spectral type. Spectral typing accuracy increases with the number of colors used in the analysis, which is virtually the same as having a well defined SED for each possible candidate. The J-H and H-K colors for T dwarfs become bluer with increasing spectral subtype, becoming degenerate with the colors of higher mass K and M dwarfs (Patten et al. 2006). IRAC/Spizer data are fundamental to break the degeneracy amongst different types shown in the near-IR. The four IRAC channels include the CH4 fundamental absorption at 3.3 microns, the continuum peak that is present for all objects cooler than 3000 K and the CO absorption at 4.7 microns, the H2O absorption in the 5.8 micron band and CH4 absorption in the 8 micron band.

We propose use the VO capabilities to perform a search for late M, L and T dwarf members in Orion based on the characterization of their SEDs. They will be constructed using data from UKIRT Deep Sky Survey (UKIDSS) and IRAC/Spitzer. We propose to compare the SED of all objects in the studied area with template observed SED’s of late L and T dwarfs using a least-squares minimization method similar to that proposed by the Bayo et al. 2008. They developed a tool (VOSA) within the VO to analyze and compare SEDs of sub-stellar objects with theoretical models. A similar study to Caballero et al. (2007) but in a more extended area could be done in the frame of the VO-AIDA 2009 School. The use of the SED-fitting method for detection of L and T’s using VO tools could be tested directly in the Sigma Orionis cluster, since despite the detailed work by Caballero et al., the full population of IPMOs is not known to its completeness. The method can also be tested on a different young cluster in Orion, like Epsilon Orionis or Delta Orionis. We expect that with the SED-minimization technique we can improve the detection efficiency of IPMOs in young clusters and find some new candidates that may remain uncovered from color-based searches. This scientific case will fully exploit the goals of the VO-AIDA 2009 School, since it will require amongst others the use of catalogue and table handling, image and spectra handling and least-squares minimization of large amounts of data. This project will need to make full use of ALADDIN, TOPCAT and VOSA amongst other VO tools. For the spectral-fitting step, we would ideally use VOSA to fit to template observed spectra, although good results can also be obtained by fitting to model spectra.

Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
Added:
>
>
  • (6) VOSA (Added by Enrique 02Mar)
 

Participants

Alvarez Iglesias, Zloczewski, Valdivielso, Hacar, Sanchez Ayaso, Kovacevic, Oreiro, Santander Vela

-- EvanthiaHatziminaoglou - 24 Feb 2009

Revision 325 Feb 2009 - Main.PaoloPadovani

Changed:
<
<

EuroVO-AIDA School 2009

>
>

EuroVO-AIDA School 2009

 

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI

Title blabla

Changed:
<
<
  • (1) Aladin
  • (2) TOPCAT
  • (3) SPLAT-VO
>
>
Tools
  • (1) VODesktop
  • (2) VOSpec
Added:
>
>
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
  • (6) VirGO
Participants

D'Odorico, Nikolajuk, Dubinovska, Suhada, Tremou, Toribio, Tundo, Perez Torres, Marchetti, De Boni, Heraudeau

 

Extragalactic 2

Changed:
<
<
Tutors: Mark ALLEN, Giuseppe LONGO
>
>
Tutors: Mark ALLEN, Eduardo GONZALEZ SOLARES, Giuseppe LONGO
 
Changed:
<
<
Title blablabla
>
>
Suggestion: Eduardo's case from the VO Info Day in Lisbon (http://www.sim.ul.pt/WorkshopVO-pt2008/prog/prog.html)
 
Added:
>
>
Tools
 
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
Changed:
<
<
  • (4) whatever else
>
>
  • (4) Aladin
Added:
>
>
  • (5) Topcat

Participants

Leitet, Messias, Finet, Tepper Garcia, Baldi, Guelbenzu, Fritz, Vulcani, Cassara', Chon, Bonchi
 

Galactic 1

Changed:
<
<
Tutors: Deborah BAINES, Nick WALTON
>
>
Tutors: Deborah BAINES, Nick WALTON
 
Changed:
<
<
Title blabla
>
>
Suggestion: use the IMF case developed by Evanthia, based on the VO-TECH Science Framework Document (see http://www.euro-vo.org/pub/fc/workflows/IMF.htm)
Added:
>
>
Tools
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) Aladin
  • (5) Topcat
Participants
 
Changed:
<
<
  • (1) Aladin
>
>
Belcheva, Tuvikene, Eisenbeiss, Graefe, Follert, Raddi, Nikolov, Borisova, Stiele, Tempel
Deleted:
<
<
  • (2) TOPCAT
  • (3) SPLAT-VO
 

Galactic 2

Changed:
<
<
Tutors: Caroline BOT, Enrique SOLANO
>
>
Tutors: Caroline BOT, Enrique SOLANO, Sebastien DERRIERE
 
Changed:
<
<
Title blablabla
>
>
Possible science case (from Alvarez Iglesias's case):
 
Added:
>
>
We propose to search for L and T candidate members in very young clusters (<10Myr) using data from UKIRT Deep Sky Survey (UKIDSS) and IRAC/Spitzer and a new method based on their Spectral Energy Distribution (SED) characterization.

The knowledge of the complete census of substellar objects in star forming regions with masses below the Deuterium burning limit (M=13 M_Jupiter, Saumon et al. 1996), nicknamed isolated planetary-mass objects (IPMOs) is very important to understand the formation processes of such low mass bodies. The origin of both IPMOs and PMOs around stars remains uncertain. It is likely that IPMOs form as a natural extension of the process that leads to the formation of low-mass stars and, probably, brown dwarfs, but they could also originate in proto-planetary discs and be ejected through dynamical interactions (e.g. Reipurth & Clarke 2001). One example of the usefulness of these searches is the deep photometric study by Caballero et al (2007) in the young (~3 Myr) and relatively close (~350 pc) Sigma Orionis cluster. In this case, they combined optical, near- and mid-IR data to characterize the sub-stellar population of the cluster down to ~ 5 M_J (~M6-L6) in an area of 790 arcmin^2. Their study indicates that both brown dwarfs and IPMOs could form as an extension of the low-mass star formation process.

An optical, near-infrared and mid-infrared photometric study on field M to T dwarfs is shown in Patten et al (2006). In this case, photometry from the Sloan Digital Sky Survey and IRAC/Spitzer was used to analyze the colors of 86 sources. They show that single colors are insufficient to determine univocally the spectral type. Spectral typing accuracy increases with the number of colors used in the analysis, which is virtually the same as having a well defined SED for each possible candidate. The J-H and H-K colors for T dwarfs become bluer with increasing spectral subtype, becoming degenerate with the colors of higher mass K and M dwarfs (Patten et al. 2006). IRAC/Spizer data are fundamental to break the degeneracy amongst different types shown in the near-IR. The four IRAC channels include the CH4 fundamental absorption at 3.3 microns, the continuum peak that is present for all objects cooler than 3000 K and the CO absorption at 4.7 microns, the H2O absorption in the 5.8 micron band and CH4 absorption in the 8 micron band.

We propose use the VO capabilities to perform a search for late M, L and T dwarf members in Orion based on the characterization of their SEDs. They will be constructed using data from UKIRT Deep Sky Survey (UKIDSS) and IRAC/Spitzer. We propose to compare the SED of all objects in the studied area with template observed SED’s of late L and T dwarfs using a least-squares minimization method similar to that proposed by the Bayo et al. 2008. They developed a tool (VOSA) within the VO to analyze and compare SEDs of sub-stellar objects with theoretical models. A similar study to Caballero et al. (2007) but in a more extended area could be done in the frame of the VO-AIDA 2009 School. The use of the SED-fitting method for detection of L and T’s using VO tools could be tested directly in the Sigma Orionis cluster, since despite the detailed work by Caballero et al., the full population of IPMOs is not known to its completeness. The method can also be tested on a different young cluster in Orion, like Epsilon Orionis or Delta Orionis. We expect that with the SED-minimization technique we can improve the detection efficiency of IPMOs in young clusters and find some new candidates that may remain uncovered from color-based searches. This scientific case will fully exploit the goals of the VO-AIDA 2009 School, since it will require amongst others the use of catalogue and table handling, image and spectra handling and least-squares minimization of large amounts of data. This project will need to make full use of ALADDIN, TOPCAT and VOSA amongst other VO tools. For the spectral-fitting step, we would ideally use VOSA to fit to template observed spectra, although good results can also be obtained by fitting to model spectra.

Tools
 
  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
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  • (4) whatever else
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  • (4) Aladin
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  • (5) Topcat

Participants

Alvarez Iglesias, Zloczewski, Valdivielso, Hacar, Sanchez Ayaso, Kovacevic, Oreiro, Santander Vela

  -- EvanthiaHatziminaoglou - 24 Feb 2009

Revision 225 Feb 2009 - Main.EvanthiaHatziminaoglou

Added:
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EuroVO-AIDA School 2009

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI

Title blabla

  • (1) Aladin
  • (2) TOPCAT
  • (3) SPLAT-VO

Extragalactic 2

Tutors: Mark ALLEN, Giuseppe LONGO

Title blablabla

  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) whatever else

Galactic 1

Tutors: Deborah BAINES, Nick WALTON

Title blabla

  • (1) Aladin
  • (2) TOPCAT
  • (3) SPLAT-VO

Galactic 2

Tutors: Caroline BOT, Enrique SOLANO

Title blablabla

  • (1) VODesktop
  • (2) VOSpec
  • (3) scripts
  • (4) whatever else
 -- EvanthiaHatziminaoglou - 24 Feb 2009

Revision 124 Feb 2009 - Main.EvanthiaHatziminaoglou

 -- EvanthiaHatziminaoglou - 24 Feb 2009
 
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