Difference: VOSchool09 (1 vs. 13)

EuroVO-AIDA School 2009

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EuroVO-AIDA School 2009

Tools

• Aladin
• VODesktop
• TOPCAT
• STILTS
• VOSpec
• SPLAT
• VOSED
• VOSA
• scripting with Python
• VirGO
  

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

EuroVO-AIDA School 2009

Tools

• Aladin
• VODesktop
• TOPCAT
• STILTS
• VOSpec
• SPLAT
• VOSED
• VOSA

• VirGO
  

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

EuroVO-AIDA School 2009

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI

Participants

Extragalactic 2

Participants

Galactic 1

Tutors: Deborah BAINES, Nick WALTON

Participants

Galactic 2

Tutors: Caroline BOT, Enrique SOLANO, Sebastien DERRIERE

Participants

-- EvanthiaHatziminaoglou - 24 Feb 2009

EuroVO-AIDA School 2009

Tools

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

Participants

Extragalactic 2

Tutors: Mark ALLEN, Eduardo GONZALEZ SOLARES, Giuseppe LONGO

Galactic 1

Tutors: Deborah BAINES, Nick WALTON

Participants

Galactic 2

Tutors: Caroline BOT, Enrique SOLANO, Sebastien DERRIERE

Participants

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
• ??

Tools

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

Participants

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

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

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

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
• ??

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

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

EuroVO-AIDA School 2009

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI

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

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

EuroVO-AIDA School 2009

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI

Tools

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

Participants

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

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

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

Participants

EuroVO-AIDA School 2009

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI

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)

Tools

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

Participants

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

Participants

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

-- EvanthiaHatziminaoglou - 24 Feb 2009

Working Groups

Extragalactic 1

Tutors: Evanthia HATZIMINAOGLOU, Paolo PADOVANI

Title blabla

Extragalactic 2

• (1) VODesktop
• (2) VOSpec
• (3) scripts

Galactic 1

Galactic 2

• (1) VODesktop
• (2) VOSpec
• (3) scripts