Stars in the Hubble Ultra Deep Field

N. Pirzkal, K. C. Sahu, A. Burgasser, L. A. Moustakas, C. Xu, S. Malhotra, J. E. Rhoads, A. M. Koekemoer, E. P. Nelan, Rogier Windhorst, N. Panagia, C. Gronwall, A. Pasquali, J. R. Walsh

Research output: Contribution to journalArticle

44 Citations (Scopus)

Abstract

We identified 46 unresolved source candidates in the Hubble Ultra Deep Field (HUDF) down to i775 = 29.5. Unresolved objects were identified using a parameter S, which measures the deviation from the curve of growth of a point source. Extensive testing of this parameter was carried out, including the effects of decreasing signal-to-noise ratio and of the apparent motions of stars, which demonstrated that stars brighter than i775 = 27.0 could be robustly identified. Low-resolution grism spectra of the 28 objects brighter than i775 = 27.0 identify 18 M and later stellar type dwarfs, two candidate L dwarfs, two QSOs, and four white dwarfs. Using the observed population of dwarfs with spectral type M4 or later, we derive a Galactic disk scale height of 400 ±100 pc for M and L stars. The local white dwarf density is computed to be as high as (1.1 ± 0.3) × 10-2 stars pc-3. On the basis of observations taken 73 days apart, we determined that no object in the field has a proper motion larger than 0″.027 yr-1 (3 σ detection limit). No high-velocity white dwarfs were identified in the HUDF, and all four candidates appear more likely to be part of the Galactic thick disk. The lack of detected halo white dwarfs implies that if the dark matter halo is 12 Gyr old, white dwarfs account for less than 10% of the dark matter halo mass.

Original languageEnglish (US)
Pages (from-to)319-332
Number of pages14
JournalAstrophysical Journal
Volume622
Issue number1 I
DOIs
StatePublished - Mar 20 2005

Fingerprint

stars
halos
signal-to-noise ratio
point source
dark matter
M stars
scale height
proper motion
quasars
point sources
signal to noise ratios
deviation
parameter
curves
effect
detection

Keywords

  • Galaxy: disk
  • Galaxy: stellar content
  • Galaxy: structure
  • Stars: late-type
  • White dwarfs

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Pirzkal, N., Sahu, K. C., Burgasser, A., Moustakas, L. A., Xu, C., Malhotra, S., ... Walsh, J. R. (2005). Stars in the Hubble Ultra Deep Field. Astrophysical Journal, 622(1 I), 319-332. https://doi.org/10.1086/427896

Stars in the Hubble Ultra Deep Field. / Pirzkal, N.; Sahu, K. C.; Burgasser, A.; Moustakas, L. A.; Xu, C.; Malhotra, S.; Rhoads, J. E.; Koekemoer, A. M.; Nelan, E. P.; Windhorst, Rogier; Panagia, N.; Gronwall, C.; Pasquali, A.; Walsh, J. R.

In: Astrophysical Journal, Vol. 622, No. 1 I, 20.03.2005, p. 319-332.

Research output: Contribution to journalArticle

Pirzkal, N, Sahu, KC, Burgasser, A, Moustakas, LA, Xu, C, Malhotra, S, Rhoads, JE, Koekemoer, AM, Nelan, EP, Windhorst, R, Panagia, N, Gronwall, C, Pasquali, A & Walsh, JR 2005, 'Stars in the Hubble Ultra Deep Field', Astrophysical Journal, vol. 622, no. 1 I, pp. 319-332. https://doi.org/10.1086/427896
Pirzkal N, Sahu KC, Burgasser A, Moustakas LA, Xu C, Malhotra S et al. Stars in the Hubble Ultra Deep Field. Astrophysical Journal. 2005 Mar 20;622(1 I):319-332. https://doi.org/10.1086/427896
Pirzkal, N. ; Sahu, K. C. ; Burgasser, A. ; Moustakas, L. A. ; Xu, C. ; Malhotra, S. ; Rhoads, J. E. ; Koekemoer, A. M. ; Nelan, E. P. ; Windhorst, Rogier ; Panagia, N. ; Gronwall, C. ; Pasquali, A. ; Walsh, J. R. / Stars in the Hubble Ultra Deep Field. In: Astrophysical Journal. 2005 ; Vol. 622, No. 1 I. pp. 319-332.
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AU - Malhotra, S.

AU - Rhoads, J. E.

AU - Koekemoer, A. M.

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AU - Windhorst, Rogier

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N2 - We identified 46 unresolved source candidates in the Hubble Ultra Deep Field (HUDF) down to i775 = 29.5. Unresolved objects were identified using a parameter S, which measures the deviation from the curve of growth of a point source. Extensive testing of this parameter was carried out, including the effects of decreasing signal-to-noise ratio and of the apparent motions of stars, which demonstrated that stars brighter than i775 = 27.0 could be robustly identified. Low-resolution grism spectra of the 28 objects brighter than i775 = 27.0 identify 18 M and later stellar type dwarfs, two candidate L dwarfs, two QSOs, and four white dwarfs. Using the observed population of dwarfs with spectral type M4 or later, we derive a Galactic disk scale height of 400 ±100 pc for M and L stars. The local white dwarf density is computed to be as high as (1.1 ± 0.3) × 10-2 stars pc-3. On the basis of observations taken 73 days apart, we determined that no object in the field has a proper motion larger than 0″.027 yr-1 (3 σ detection limit). No high-velocity white dwarfs were identified in the HUDF, and all four candidates appear more likely to be part of the Galactic thick disk. The lack of detected halo white dwarfs implies that if the dark matter halo is 12 Gyr old, white dwarfs account for less than 10% of the dark matter halo mass.

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