E. Solano¹, N. Lodieu², M. Aberasturi¹,

M.R. Zapatero-Osorio¹, E. Martín¹

1.- Centro de Astrobiología (INTA-CSIC), Madrid, Spain

2.- Instituto de Astrofísica de Canarias, Tenerife, Spain

Discovery of ultracool subdwarfs

using Virtual Observatory tools

Ultracool subdwarfs: properties

• Metal-poor dwarfs with spectral type later than M7.Metal-poor dwarfs with spectral type later than M7.

• Less luminous (actually hotter) than their solar-metallicity Less luminous (actually hotter) than their solar-metallicity

counterparts due to the dearth of metals in their atmospheres.counterparts due to the dearth of metals in their atmospheres.

• Metal-poor dwarfs with spectral type later than M7.Metal-poor dwarfs with spectral type later than M7.

• Less luminous (actually hotter) than their solar-metallicity Less luminous (actually hotter) than their solar-metallicity

counterparts due to the dearth of metals in their atmospheres.counterparts due to the dearth of metals in their atmospheres.

Ultracool subdwarfs: Identification

• Halo regionsHalo regions

• No contamination by disk stars.No contamination by disk stars.

• Low luminosity.Low luminosity.

• Trigonometrical parallaxes and spectra unobtainable.Trigonometrical parallaxes and spectra unobtainable.

• Solar neighbourhoodSolar neighbourhood

• Low luminosity.Low luminosity.

• Hard to find because of their local scarcity (4 out of 348 at d<10 pc, Henry Hard to find because of their local scarcity (4 out of 348 at d<10 pc, Henry

et al. 2006, AJ, 132, 2360). et al. 2006, AJ, 132, 2360).

• Halo regionsHalo regions

• No contamination by disk stars.No contamination by disk stars.

• Low luminosity.Low luminosity.

• Trigonometrical parallaxes and spectra unobtainable.Trigonometrical parallaxes and spectra unobtainable.

• Solar neighbourhoodSolar neighbourhood

• Low luminosity.Low luminosity.

• Hard to find because of their local scarcity (4 out of 348 at d<10 pc, Henry Hard to find because of their local scarcity (4 out of 348 at d<10 pc, Henry

et al. 2006, AJ, 132, 2360). et al. 2006, AJ, 132, 2360).

Henry et al.

Ultracool subdwarfs: Identification

• Key parameter: Key parameter: Proper motionProper motion

• The high space velocities of subdwarfs allow them to distinguish The high space velocities of subdwarfs allow them to distinguish

from the multitude of similarly faint but slowly moving disk stars.from the multitude of similarly faint but slowly moving disk stars.

• Key parameter: Key parameter: Proper motionProper motion

• The high space velocities of subdwarfs allow them to distinguish The high space velocities of subdwarfs allow them to distinguish

from the multitude of similarly faint but slowly moving disk stars.from the multitude of similarly faint but slowly moving disk stars.

Ultracool subdwarfs: Identification (II)

• DrawbackDrawback

• Identification typically requires the combination of Identification typically requires the combination of

attributes (colors, proper motions,...) available from attributes (colors, proper motions,...) available from

different archives of large-area surveys (e.g. UKIDSS, different archives of large-area surveys (e.g. UKIDSS,

SDSS, 2MASS, DENIS,...). SDSS, 2MASS, DENIS,...).

• Very time-consuming task if performed by hand but, on Very time-consuming task if performed by hand but, on

the contrary, an approach that perfectly fits in the the contrary, an approach that perfectly fits in the

framework of the Virtual Observatory. framework of the Virtual Observatory.

• DrawbackDrawback

• Identification typically requires the combination of Identification typically requires the combination of

attributes (colors, proper motions,...) available from attributes (colors, proper motions,...) available from

different archives of large-area surveys (e.g. UKIDSS, different archives of large-area surveys (e.g. UKIDSS,

SDSS, 2MASS, DENIS,...). SDSS, 2MASS, DENIS,...).

• Very time-consuming task if performed by hand but, on Very time-consuming task if performed by hand but, on

the contrary, an approach that perfectly fits in the the contrary, an approach that perfectly fits in the

framework of the Virtual Observatory. framework of the Virtual Observatory.

The Virtual Observatory (VO)

• VO is a consolidated initiative that represents the framework where to VO is a consolidated initiative that represents the framework where to

develop archive-based research.develop archive-based research.

• By ensuring easy and transparent access to astronomical resources By ensuring easy and transparent access to astronomical resources

the Virtual Observatory is fostering new and/or more efficient science. the Virtual Observatory is fostering new and/or more efficient science.

• VO is a consolidated initiative that represents the framework where to VO is a consolidated initiative that represents the framework where to

develop archive-based research.develop archive-based research.

• By ensuring easy and transparent access to astronomical resources By ensuring easy and transparent access to astronomical resources

the Virtual Observatory is fostering new and/or more efficient science. the Virtual Observatory is fostering new and/or more efficient science.

Std

s

Tools

Science

This work: Objectives

• Identification of a statistically significant number of bona-fide ultracool subdwarfs to:

Bridge the gap between M and L spectral types.

Help the discovery of cooler Population II brown dwarfs.

Establish optical and near-infrared spectral classification at

cooler temperatures and lower metallicities.

Investigate the role of metallicity in the atmospheres of

ultracool dwarfs.

Shed light on the star formation history of the Milky Way.

Good candidates for exoplanet searches (low chromospheric

activity).

• Identification of a statistically significant number of bona-fide ultracool subdwarfs to:

Bridge the gap between M and L spectral types.

Help the discovery of cooler Population II brown dwarfs.

Establish optical and near-infrared spectral classification at

cooler temperatures and lower metallicities.

Investigate the role of metallicity in the atmospheres of

ultracool dwarfs.

Shed light on the star formation history of the Milky Way.

Good candidates for exoplanet searches (low chromospheric

activity).

This work: Methodology• Proper motion and photometric searches using VO tools (ALADIN, TOPCAT).

• 8500 (SDSS-2MASS) + 1500 (SDSS-UKIDSS) square degrees explored.

• Proper motion and photometric searches using VO tools (ALADIN, TOPCAT).

• 8500 (SDSS-2MASS) + 1500 (SDSS-UKIDSS) square degrees explored.

This work: Methodology (II)

• Workflow:

All point sources in SDSS without 2MASS/UKIDSS counterparts within 5”.

Colours and reduced proper motion based on the M7-M9.5 subdwarfs identified by Lépine & Scholz (2008, AJ, 681, L33).

(J-K) ≤ 0.7 mag

• Workflow:

All point sources in SDSS without 2MASS/UKIDSS counterparts within 5”.

Colours and reduced proper motion based on the M7-M9.5 subdwarfs identified by Lépine & Scholz (2008, AJ, 681, L33).

(J-K) ≤ 0.7 mag

This work: Results

• SDSS (Data Release 7) - 2MASS (Point Source Catalogue)

candidates after the initial search 356

Further refinement

Whenever possible, UKIDSS and SuperCosmos were used for -.a third epoch

.Visual inspection to discard false detections -

.Final number of candidates: 30. Six were already known

:Optical spectroscopic follow-up of new candidates

,candidates observed with NOT/ALFOSC in January 6 = 2 + 1 + 3 -.July and August 2009

.out of 6 exhibit spectral features typical of subdwarfs 6 -

• SDSS (Data Release 7) - 2MASS (Point Source Catalogue)

356 candidates after the initial search

Further refinement

- Whenever possible, UKIDSS and SuperCosmos were used for a third epoch.

- Visual inspection to discard false detections.

Final number of candidates: 30. Six were already known.

Optical spectroscopic follow-up of new candidates:

- 3 + 1 + 2 = 6 candidates observed with NOT/ALFOSC in January, July and August 2009.

- 6 out of 6 exhibit spectral features typical of subdwarfs.

This work: Results (II)• SDSS (Data Release 7) – UKIDSS /LAS (Data Release 5)

Aim: Detection of cooler (down to 1000K) and less massive (up to Jupiter masses) subdwarfs in a radius of 25 pc assuming [Fe/H] 60 .1- =

new candidates 31 after removal of false detections and known) (subdwarfs

:Optical spectroscopic follow-up

GTC / OSIRIS

.hours awarded in semester 09A 11

objects observed but S/N lower than expected. Very hard to 8 -.confirm/discard candidates

hours awarded in 09B 16.objects sent to the queue 19

VLT / FORS2

hours 20.objects sent to the queue for the next semester 22

• SDSS (Data Release 7) – UKIDSS /LAS (Data Release 5)

Aim: Detection of cooler (down to 1000K) and less massive (up to 60 Jupiter masses) subdwarfs in a radius of 25 pc assuming [Fe/H] = -1.

31 new candidates (after removal of false detections and known subdwarfs)

Optical spectroscopic follow-up:

GTC / OSIRIS

11 hours awarded in semester 09A.

- 8 objects observed but S/N lower than expected. Very hard to confirm/discard candidates.

16 hours awarded in 09B 19 objects sent to the queue.

VLT / FORS2

20 hours 22 objects sent to the queue for the next semester.

Summary

• The census of ultracool subdwarfs is largely incomplete.

39 out of which only three show L-types.

• We have developed a methodology to identify ultracool .subdwarfs using Virtual Observatory tools

• .Six confirmed subdwarfs out of six observed spectroscopically

- Spectral types: M5-M6 (only the brightest targets – SDSS / 2MASS

.(have been analysed so far

• If the success rate remains so for fainter objects our procedure will.double the number of subdwarfs with spectral types later than M7

• This methodology opens new prospects to further increase these,numbers using upcoming large-scale surveys (VISTA, PanSTARRS.(…

• The census of ultracool subdwarfs is largely incomplete.

39 out of which only three show L-types.

• We have developed a methodology to identify ultracool subdwarfs using Virtual Observatory tools.

• Six confirmed subdwarfs out of six observed spectroscopically.

Spectral types: M5-M6 (only the brightest targets – SDSS / 2MASS -

have been analysed so far).

• If the success rate remains so for fainter objects our procedure will double the number of subdwarfs with spectral types later than M7.

• This methodology opens new prospects to further increase these numbers using upcoming large-scale surveys (VISTA, PanSTARRS,…).