The WFC3 galactic bulge treasury program: A first look at resolved stellar population tools

Thomas M. Brown, Kailash Sahu, Manuela Zoccali, Alvio Renzini, Henry C. Ferguson, Jay Anderson, Ed Smith, Howard E. Bond, Dante Minniti, Jeff A. Valenti, Stefano Casertano, Mario Livio, Nino Panagia, Don A. Vandenberg, Elena Valenti

Resultado de la investigación: Article

16 Citas (Scopus)

Resumen

When the Wide Field Camera 3 (WFC3) is installed on the Hubble Space Telescope (HST), the astronomical community will have access to powerful new capabilities for investigating resolved stellar populations. The WFC3 Galactic Bulge Treasury program will obtain deep imaging in five photometric bands on four low-extinction fields. These data will have no proprietary period, and will enable a variety of science investigations not possible with previous data sets. To aid in planning for the use of these data and for future observing proposals, we provide an introduction to the Treasury program, its photometric system, and the associated calibration effort. The observing strategy is based upon a new photometric system employing five WFC3 bands spanning the UV, optical, and near-infrared: F390W, F555W, F814W, F110W, and F160W (analogous but not identical to the ground-based filters Washington C, V, I, J, and H). With these bands, one can construct reddening-free indices of temperature and metallicity. Using this photometric system, the program will target six fields in well studied star clusters, spanning a wide range of metallicity, and four fields in low-extinction windows of the Galactic bulge. The cluster data serve to calibrate the reddening-free indices, provide empirical population templates, and correct the transformation of theoretical isochrone libraries into the WFC3 photometric system. The bulge data will shed light on the bulge formation history, and will also serve as empirical population templates for other studies. One of the fields includes 12 candidate hosts of extrasolar planets. Color-magnitude diagrams (CMDs) are the most popular tool for analyzing resolved stellar populations. However, due to degeneracies among temperature, metallicity, and reddening in traditional CMDs, it can be difficult to draw robust conclusions from the data. The five-band system used for the bulge Treasury observations will provide reddening-free indices that are roughly orthogonal in temperature and metallicity, and we argue that model fitting in an index-index diagram will make better use of the information than fitting separate CMDs. We provide some results from simulations to show the expected quality of the data and their potential for differentiating between different star formation histories.

Idioma originalEnglish
Páginas (desde-hasta)3172-3180
Número de páginas9
PublicaciónAstronomical Journal
Volumen137
N.º2
DOI
EstadoPublished - 2009

Huella dactilar

galactic bulge
cameras
metallicity
color-magnitude diagram
diagram
extinction
templates
histories
star clusters
extrasolar planets
Hubble Space Telescope
temperature
planning
proposals
star formation
history
diagrams
programme
aid
near infrared

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Citar esto

Brown, T. M., Sahu, K., Zoccali, M., Renzini, A., Ferguson, H. C., Anderson, J., ... Valenti, E. (2009). The WFC3 galactic bulge treasury program: A first look at resolved stellar population tools. Astronomical Journal, 137(2), 3172-3180. https://doi.org/10.1088/0004-6256/137/2/3172
Brown, Thomas M. ; Sahu, Kailash ; Zoccali, Manuela ; Renzini, Alvio ; Ferguson, Henry C. ; Anderson, Jay ; Smith, Ed ; Bond, Howard E. ; Minniti, Dante ; Valenti, Jeff A. ; Casertano, Stefano ; Livio, Mario ; Panagia, Nino ; Vandenberg, Don A. ; Valenti, Elena. / The WFC3 galactic bulge treasury program : A first look at resolved stellar population tools. En: Astronomical Journal. 2009 ; Vol. 137, N.º 2. pp. 3172-3180.
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abstract = "When the Wide Field Camera 3 (WFC3) is installed on the Hubble Space Telescope (HST), the astronomical community will have access to powerful new capabilities for investigating resolved stellar populations. The WFC3 Galactic Bulge Treasury program will obtain deep imaging in five photometric bands on four low-extinction fields. These data will have no proprietary period, and will enable a variety of science investigations not possible with previous data sets. To aid in planning for the use of these data and for future observing proposals, we provide an introduction to the Treasury program, its photometric system, and the associated calibration effort. The observing strategy is based upon a new photometric system employing five WFC3 bands spanning the UV, optical, and near-infrared: F390W, F555W, F814W, F110W, and F160W (analogous but not identical to the ground-based filters Washington C, V, I, J, and H). With these bands, one can construct reddening-free indices of temperature and metallicity. Using this photometric system, the program will target six fields in well studied star clusters, spanning a wide range of metallicity, and four fields in low-extinction windows of the Galactic bulge. The cluster data serve to calibrate the reddening-free indices, provide empirical population templates, and correct the transformation of theoretical isochrone libraries into the WFC3 photometric system. The bulge data will shed light on the bulge formation history, and will also serve as empirical population templates for other studies. One of the fields includes 12 candidate hosts of extrasolar planets. Color-magnitude diagrams (CMDs) are the most popular tool for analyzing resolved stellar populations. However, due to degeneracies among temperature, metallicity, and reddening in traditional CMDs, it can be difficult to draw robust conclusions from the data. The five-band system used for the bulge Treasury observations will provide reddening-free indices that are roughly orthogonal in temperature and metallicity, and we argue that model fitting in an index-index diagram will make better use of the information than fitting separate CMDs. We provide some results from simulations to show the expected quality of the data and their potential for differentiating between different star formation histories.",
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author = "Brown, {Thomas M.} and Kailash Sahu and Manuela Zoccali and Alvio Renzini and Ferguson, {Henry C.} and Jay Anderson and Ed Smith and Bond, {Howard E.} and Dante Minniti and Valenti, {Jeff A.} and Stefano Casertano and Mario Livio and Nino Panagia and Vandenberg, {Don A.} and Elena Valenti",
year = "2009",
doi = "10.1088/0004-6256/137/2/3172",
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Brown, TM, Sahu, K, Zoccali, M, Renzini, A, Ferguson, HC, Anderson, J, Smith, E, Bond, HE, Minniti, D, Valenti, JA, Casertano, S, Livio, M, Panagia, N, Vandenberg, DA & Valenti, E 2009, 'The WFC3 galactic bulge treasury program: A first look at resolved stellar population tools', Astronomical Journal, vol. 137, n.º 2, pp. 3172-3180. https://doi.org/10.1088/0004-6256/137/2/3172

The WFC3 galactic bulge treasury program : A first look at resolved stellar population tools. / Brown, Thomas M.; Sahu, Kailash; Zoccali, Manuela; Renzini, Alvio; Ferguson, Henry C.; Anderson, Jay; Smith, Ed; Bond, Howard E.; Minniti, Dante; Valenti, Jeff A.; Casertano, Stefano; Livio, Mario; Panagia, Nino; Vandenberg, Don A.; Valenti, Elena.

En: Astronomical Journal, Vol. 137, N.º 2, 2009, p. 3172-3180.

Resultado de la investigación: Article

TY - JOUR

T1 - The WFC3 galactic bulge treasury program

T2 - A first look at resolved stellar population tools

AU - Brown, Thomas M.

AU - Sahu, Kailash

AU - Zoccali, Manuela

AU - Renzini, Alvio

AU - Ferguson, Henry C.

AU - Anderson, Jay

AU - Smith, Ed

AU - Bond, Howard E.

AU - Minniti, Dante

AU - Valenti, Jeff A.

AU - Casertano, Stefano

AU - Livio, Mario

AU - Panagia, Nino

AU - Vandenberg, Don A.

AU - Valenti, Elena

PY - 2009

Y1 - 2009

N2 - When the Wide Field Camera 3 (WFC3) is installed on the Hubble Space Telescope (HST), the astronomical community will have access to powerful new capabilities for investigating resolved stellar populations. The WFC3 Galactic Bulge Treasury program will obtain deep imaging in five photometric bands on four low-extinction fields. These data will have no proprietary period, and will enable a variety of science investigations not possible with previous data sets. To aid in planning for the use of these data and for future observing proposals, we provide an introduction to the Treasury program, its photometric system, and the associated calibration effort. The observing strategy is based upon a new photometric system employing five WFC3 bands spanning the UV, optical, and near-infrared: F390W, F555W, F814W, F110W, and F160W (analogous but not identical to the ground-based filters Washington C, V, I, J, and H). With these bands, one can construct reddening-free indices of temperature and metallicity. Using this photometric system, the program will target six fields in well studied star clusters, spanning a wide range of metallicity, and four fields in low-extinction windows of the Galactic bulge. The cluster data serve to calibrate the reddening-free indices, provide empirical population templates, and correct the transformation of theoretical isochrone libraries into the WFC3 photometric system. The bulge data will shed light on the bulge formation history, and will also serve as empirical population templates for other studies. One of the fields includes 12 candidate hosts of extrasolar planets. Color-magnitude diagrams (CMDs) are the most popular tool for analyzing resolved stellar populations. However, due to degeneracies among temperature, metallicity, and reddening in traditional CMDs, it can be difficult to draw robust conclusions from the data. The five-band system used for the bulge Treasury observations will provide reddening-free indices that are roughly orthogonal in temperature and metallicity, and we argue that model fitting in an index-index diagram will make better use of the information than fitting separate CMDs. We provide some results from simulations to show the expected quality of the data and their potential for differentiating between different star formation histories.

AB - When the Wide Field Camera 3 (WFC3) is installed on the Hubble Space Telescope (HST), the astronomical community will have access to powerful new capabilities for investigating resolved stellar populations. The WFC3 Galactic Bulge Treasury program will obtain deep imaging in five photometric bands on four low-extinction fields. These data will have no proprietary period, and will enable a variety of science investigations not possible with previous data sets. To aid in planning for the use of these data and for future observing proposals, we provide an introduction to the Treasury program, its photometric system, and the associated calibration effort. The observing strategy is based upon a new photometric system employing five WFC3 bands spanning the UV, optical, and near-infrared: F390W, F555W, F814W, F110W, and F160W (analogous but not identical to the ground-based filters Washington C, V, I, J, and H). With these bands, one can construct reddening-free indices of temperature and metallicity. Using this photometric system, the program will target six fields in well studied star clusters, spanning a wide range of metallicity, and four fields in low-extinction windows of the Galactic bulge. The cluster data serve to calibrate the reddening-free indices, provide empirical population templates, and correct the transformation of theoretical isochrone libraries into the WFC3 photometric system. The bulge data will shed light on the bulge formation history, and will also serve as empirical population templates for other studies. One of the fields includes 12 candidate hosts of extrasolar planets. Color-magnitude diagrams (CMDs) are the most popular tool for analyzing resolved stellar populations. However, due to degeneracies among temperature, metallicity, and reddening in traditional CMDs, it can be difficult to draw robust conclusions from the data. The five-band system used for the bulge Treasury observations will provide reddening-free indices that are roughly orthogonal in temperature and metallicity, and we argue that model fitting in an index-index diagram will make better use of the information than fitting separate CMDs. We provide some results from simulations to show the expected quality of the data and their potential for differentiating between different star formation histories.

KW - Brown dwarfs

KW - Galaxy: bulge

KW - Galaxy: formation

KW - Galaxy: stellar content

KW - Globular clusters: individual (M92, NGC6752, 47 Tuc, NGC5927, NGC6528, NGC6791)

KW - Stars: low-mass

KW - Techniques: photometric

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