Stellar Populations and Formation Histories of Massive Galaxies Derived from Deep Hubble Space Telescope Grism Data
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Grism
Hubble Ultra-Deep Field
Space observatory
Observational cosmology
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We study the rest-frame ultra-violet sizes of massive (~0.8 x 10^11 M_Sun) galaxies at 3.45 x, between 2
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We have used HST WFPC-2 observations of five fields along the eastern spiral arm regions of M31 to study the stellar populations. We use fits to stellar models to determine extinction individually for the stars in OB associations in these fields. The range of extinction within each cluster is the major constraint on our ability to determine accurate parameters for each association. We are able to determine ages of the clusters to ∼0.2 in log age, which is sufficient to distinguish between the older and younger associations. These observations provide us with the first measurement of the ages of young star clouds in M31 and allow us to make comparisons with other, less well-calibrated tracers of the association ages, in particular the Ha and H i morphologies.
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view Abstract Citations (76) References (37) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Redshift Z approximately 1 Field Galaxies Observed with the Keck Telescope and the Hubble Space Telescope Koo, David C. ; Vogt, Nicole P. ; Phillips, Andrew C. ; Guzman, Rafael ; Wu, K. L. ; Faber, S. M. ; Gronwall, Caryl ; Forbes, Duncan A. ; Illingworth, Garth D. ; Groth, Edward J. ; Davis, Marc ; Kron, Richard G. ; Szalay, Alexander S. Abstract We report results based on 35 new spectroscopic redshifts obtained with the Keck Telescope for field galaxies that also have photometry and morphology from survey images taken by the refurbished Hubble Space Telescope. A sample of 24 redshifts for galaxies fainter than I = 22 has a median redshift of z ~ 0.81. This result is inconsistent with the lower median redshift of z ~ 0.6 predicted by the "maximal merger models" of Carlberg, which otherwise fit existing data. The data match an extrapolation of the Canada France Redshift Survey (CFRS), as well as predictions of certain mild luminosity-evolution models. Nearly half of the redshifts lie in two structures at z ~ 0.81 and z ~ 1.0, showing the presence of high-density concentrations spanning scales of ~1 h^-1^ Mpc, i.e., the size of groups. We find emission lines or the presence of possible neighbors in seven of nine otherwise luminous galaxies with red central regions at redshifts beyond z ~ 0.7. We also note a diversity of morphological types among blue galaxies at z ~ 1, including small compact galaxies, "chains," and "blue nucleated galaxies." These morphologies are found among local, but generally less luminous, galaxies. Distant blue galaxies also include apparently normal late-type spirals. These findings could imply modest bursts of star formation caused by mergers or interactions of small, gas-rich galaxies with each other or with larger, well-formed galaxies. This first glimpse of very faint z ~ 1 field galaxies of diverse colors and morphologies suggests that a mixture of physical processes is at work in the formation and evolution of faint field galaxies. Publication: The Astrophysical Journal Pub Date: October 1996 DOI: 10.1086/177802 arXiv: arXiv:astro-ph/9604113 Bibcode: 1996ApJ...469..535K Keywords: COSMOLOGY: OBSERVATIONS; GALAXIES: FORMATION; GALAXIES: DISTANCES AND REDSHIFTS; GALAXIES: EVOLUTION; GALAXIES: STRUCTURE; Astrophysics E-Print: 20 pages (31 with table and GIF figures). Full text and postscript figures are available at http://www.ucolick.org/~nicole/pubs/pubs.html#gs1 and http://tarkus.pha.jhu.edu/deep/publications.html . Accepted by The Astrophysical Journal full text sources arXiv | ADS | data products SIMBAD (42) NED (41) MAST (1) ESA (1)
Hubble Ultra-Deep Field
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We have studied the stellar populations near the nucleus of the nearby spiral galaxy M33 using archival observations of the Hubble Space elescope Planetary Camera in the F555W and F785LP passbands. The I vs (V-I) color-magnitude diagram reveals a young stellar population with a blue main sequence and red supergiants, and stars in a blue loop that are Cepheid candidates. An old red giant branch is clearly visible, with a break at I = 20.7 mag which is, within the observational errors, identical to the giant branch termination point of the Mould & Kristian (1986, ApJ, 305,591) halo field. However, red giants are seen up to I= 19.5 mag, and many bright red giants are undetected in the V band. We find evidence for a wide abundance spread of at least 1.5 dex from metal- poor (~M92) to metal-rich (>= 47 Tucanae) in the Population II stars, in sharp contrast to the M33 halo field of Mould & Kristian (1986) which is metal-poor (~M92) with a narrow abundance range. We show that the various stellar populations have different spatial distributions. The Population II stars are more centrally concentrated than the Population I stars. The red giants brighter than I = 20.7 (the termination point for a Galactic globular cluster giant branch) are found to be more centrally concentrated than the (presumably) old red giants. The most-centrally concentrated bright Population II giants are probably associated with the many bright red giants that are undetected in the V band. These infrared- bright giants were probably created in an intermediate-age burst of star formation that took place well after the formation of the oldest halo stars but long before the recent burst of star formation seen in the nearby OB associations. This stellar population probably corresponds to the bulge identified in the infrared H band by Minniti et al. (1993, ApJ, 410, L79).
Hubble Ultra-Deep Field
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The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image an undistinguished field at high Galactic latitude in four passbands as deeply as reasonably possible. These images provide the most detailed view to date of distant field galaxies and are likely to be important for a wide range of studies in galaxy evolution and cosmology. In order to optimize observing in the time available, a field in the northern continuous viewing zone was selected and images were taken for ten consecutive days, or approximately 150 orbits. Shorter 1-2 orbit images were obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground- based telescopes. The observations were made from 1995 December 18-30, and both raw and reduced data have been put in the public domain as a community service. We present a summary of the criteria for selecting the field, the rationale behind the filter selection and observing times in each band, and the strategies for planning the observations to maximize the exposure time while avoiding Earth-scattered light. Data reduction procedures are outlined, and images of the combined frames in each band are presented. Objects detected in these images are listed in a catalog with their basic photometric parameters.
Data Reduction
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Space observatory
Hubble Ultra-Deep Field
Observational cosmology
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Within the Local Universe galaxies can be studied in great detail star by star, and here we review the results of quantitative studies in nearby dwarf galaxies. The color-magnitude diagram synthesis method is well established as the most accurate way to determine star-formation histories of galaxies back to the earliest times. This approach received a large boost from the exceptional data sets that wide-field CCD imagers on the ground and the Hubble Space Telescope could provide. Spectroscopic studies using large ground-based telescopes such as VLT, Magellan, Keck, and HET have allowed the determination of abundances and kinematics for significant samples of stars in nearby dwarf galaxies. These studies have shown how the properties of stellar populations can vary spatially and temporally. This leads to important constraints to theories of galaxy formation and evolution. The combination of spectroscopy and imaging and what they have taught us about dwarf galaxy formation and evolution is the aim of this review.
Local Group
Dwarf spheroidal galaxy
Dwarf galaxy problem
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The James Webb Space Telescope (JWST) will enable the detection of optical emission lines in galaxies spanning a broad range of luminosities out to redshifts z>10. Measurements of key galaxy properties, such as star formation rate and metallicity, through these observations will provide unique insight into, e.g., the role of feedback from stars and active galactic nuclei (AGNs) in regulating galaxy evolution, the co-evolution of AGNs and host galaxies, the physical origin of the 'main sequence' of star-forming galaxies and the contribution by star-forming galaxies to cosmic reionization. We present an original framework to simulate and analyse observations performed with the Near Infrared Spectrograph (NIRSpec) on board JWST. We use the BEAGLE tool (BayEsian Analysis of GaLaxy sEds) to build a semi-empirical catalogue of galaxy spectra based on photometric spectral energy distributions (SEDs) of dropout galaxies in the Hubble Ultra Deep Field (HUDF). We demonstrate that the resulting catalogue of galaxy spectra satisfies different types of observational constraints on high redshift galaxies, and use it as input to simulate NIRSpec/prism (R~100) observations. We show that a single 'deep' (~100 ks) NIRSpec/prism pointing in the HUDF will enable S/N>3 detections of multiple optical emission lines in ~30 (~60) galaxies at z>6 (z~4-6) down to m_F160W<30 AB mag. Such observations will allow measurements of galaxy star formation rates, ionization parameters and gas-phase metallicities within factors of 1.5, mass-to-light ratios within a factor of 2, galaxy ages within a factor of 3 and V-band attenuation optical depths with a precision of 0.3.
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Low resolution
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