The Hubble Space Telescope and the High Redshift Universe

10.1142/3314 ◽  
1997 ◽  
Keyword(s):  
Hubble Space Telescope ◽  
High Redshift ◽  
Space Telescope ◽  
High Redshift Universe

scholarly journals What we learn from the Frontier Fields cluster MACS J0416.1-2403

2015 ◽  
Vol 11 (A29B) ◽  
pp. 787-790
Author(s):  
S. H. Suyu ◽  
C. Grillo ◽  
P. Rosati
Keyword(s):  
Mass Distribution ◽  
Hubble Space Telescope ◽  
High Redshift ◽  
Galaxy Cluster ◽  
Essential Elements ◽  
Central Mass ◽  
Great Opportunity ◽  
Space Telescope ◽  
James Webb Space Telescope ◽  
High Redshift Universe

AbstractThe Frontier Fields cluster MACS J0416.1-2403 with its extensive imaging and spectroscopic data sets provides a great opportunity to study the mass distribution of the galaxy cluster and members, the high-redshift Universe and cosmology. By taking advantage of the observations in the 16 Hubble Space Telescope imaging bands of the Cluster Lensing And Supernova survey with Hubble (CLASH) survey and our large spectroscopic follow-up program with the VIsible Multi-Object Spectrograph (VIMOS) on the Very Large Telescope (VLT), we have been able to identify and obtain the spectroscopic redshifts of 10 important strong lensing systems in this cluster. Furthermore, we have selected and modeled the mass distribution of ~200 candidate cluster members residing in the inner regions of the cluster. We present the results on the model-predicted central mass profile and subhalo population, which are detailed in Grillo et al. (2015). Work is underway to quantify the effects of line-of-sight structures. These are essential elements to make progress in our understanding of the dark matter distribution in massive galaxy clusters and of the distant Universe within the current Frontier Fields initiative and before the advent of the James Webb Space Telescope.

scholarly journals Canada-France Redshift Survey: [ITAL]Hubble Space Telescope[/ITAL] Imaging of High-Redshift Field Galaxies

1995 ◽  
Vol 451 (1) ◽  
Author(s):  
David Schade ◽  
S. J. Lilly ◽  
David Crampton ◽  
F. Hammer ◽  
O. Le Fèvre ◽  
...  
Keyword(s):  
Hubble Space Telescope ◽  
High Redshift ◽  
Space Telescope ◽  
Redshift Survey

scholarly journals Studying the physical properties of tidal features – I. Extracting morphological substructure in CANDELS observations and VELA simulations

2019 ◽  
Vol 486 (2) ◽  
pp. 2643-2659 ◽  
Author(s):  
Kameswara Bharadwaj Mantha ◽  
Daniel H McIntosh ◽  
Cody P Ciaschi ◽  
Rubyet Evan ◽  
Henry C Ferguson ◽  
...  
Keyword(s):  
Galaxy Evolution ◽  
Hubble Space Telescope ◽  
High Redshift ◽  
Software Tool ◽  
Space Telescope ◽  
Visual Appearance ◽  
James Webb Space Telescope ◽  
Profile Fitting ◽  
Major Merger ◽  
Merger Rate

Abstract The role of major mergers in galaxy evolution remains a key open question. Existing empirical merger identification methods use non-parametric and subjective visual classifications that can pose systematic challenges to constraining merger histories. As a first step towards overcoming these challenges, we develop and share publicly a new python-based software tool that identifies and extracts the flux-wise and area-wise significant contiguous regions from the model-subtracted residual images produced by popular parametric light-profile fitting tools (e.g. galfit). Using Hubble Space Telescope (HST) H-band single-Sérsic residual images of 17 CANDELS galaxies, we demonstrate the tools ability to measure the surface brightness and improve the qualitative identification of a variety of common residual features (disc structures, spiral substructures, plausible tidal features, and strong gravitational arcs). We test our method on synthetic HST observations of a z ∼ 1.5 major merger from the VELA hydrodynamic simulations. We extract H-band residual features corresponding to the birth, growth, and fading of tidal features during different stages and viewing orientations at CANDELS depths and resolution. We find that the extracted features at shallow depths have noisy visual appearance and are susceptible to viewing angle effects. For a VELA z ∼ 3 major merger, we find that James Webb Space Telescope NIRCam observations can probe high-redshift tidal features with considerable advantage over existing HST capabilities. Further quantitative analysis of plausible tidal features extracted with our new software hold promise for the robust identification of hallmark merger signatures and corresponding improvements to merger rate constraints.

scholarly journals Outside the Lyman-break box: detecting Lyman continuum emitters at 3.5 < z < 5.1 with CLAUDS

2020 ◽  
Vol 494 (4) ◽  
pp. 4986-5007 ◽  
Author(s):  
U Meštrić ◽  
E V Ryan-Weber ◽  
J Cooke ◽  
R Bassett ◽  
M Sawicki ◽  
...  
Keyword(s):  
Intergalactic Medium ◽  
Hubble Space Telescope ◽  
High Redshift ◽  
Large Area ◽  
Redshift Range ◽  
Space Telescope ◽  
High Redshift Galaxies ◽  
Lyman Continuum ◽  
Deep Survey ◽  
Individual Galaxies

ABSTRACT Identifying non-contaminated sample of high-redshift galaxies with escaping Lyman continuum (LyC) flux is important for understanding the sources and evolution of cosmic reionization. We present CLAUDS (CFHT Large Area u-band deep survey) u-band photometry of the COSMOS field to probe LyC radiation from spectroscopically confirmed galaxies at $z$ ≥ 3.5 and outside the standard Lyman-break galaxy colour-selection expectations. Complementary to the CLAUDS data, we use Subaru multifilter photometry, Hubble Space Telescope (HST) multifilter imaging, and the spectroscopic surveys D10K, VUDS, and 3D-HST. We present a sample of Lyman continuum galaxy (LCG) candidates in the redshift range 3.5 ≲ $z$ ≲ 5.1. Here, we introduce 5 LCG candidates, where two are flagged quality 1 and three quality 2. The estimated $f_{\rm esc}^{\rm abs}$ for quality 1 candidates are in the range $\sim 5 - 73{{\ \rm per\ cent}}$ and $\sim 30 - 93{{\ \rm per\ cent}}$. These estimates are based on our derived parameters from individual galaxies as inputs to a range of BPASS models as well as mean intergalactic medium (IGM) and maximal intergalactic and circumgalactic media (IGM+CGM) transmission. We conclude that our search for LCGs is most likely biased to lines of sight with low H i densities or free from Lyman limit systems. Our two best LCG candidates have EW (Lyα) ≤ 50 Å and we find no correlation or anticorrelation between EW (Lyα), $f_{\rm esc}^{\rm abs}$, and Robs, the ratio of ionizing to non-ionizing observed flux in the measured passbands. Stacking candidates without solid LyC detections (S/N &lt; 3) results in an estimated $f_{\rm esc}^{\rm abs}$ from galaxies not greater than $1{{\ \rm per\ cent}}$.

scholarly journals Chandra and Hubble Space Telescope observations of dark gamma-ray bursts and their host galaxies

2019 ◽  
Vol 486 (3) ◽  
pp. 3105-3117 ◽  
Author(s):  
A A Chrimes ◽  
A J Levan ◽  
E R Stanway ◽  
J D Lyman ◽  
A S Fruchter ◽  
...  
Keyword(s):  
Morphological Analysis ◽  
Gamma Ray ◽  
Hubble Space Telescope ◽  
High Redshift ◽  
Host Population ◽  
Host Galaxy ◽  
Host Galaxies ◽  
Space Telescope ◽  
X Ray ◽  
Dust Component

Abstract We present a study of 21 dark gamma-ray burst (GRB) host galaxies, predominantly using X-ray afterglows obtained with the Chandra X-Ray Observatory (CXO) to precisely locate the burst in deep Hubble Space Telescope (HST) imaging of the burst region. The host galaxies are well-detected in F160W in all but one case and in F606W imaging in 60 per cent of cases. We measure magnitudes and perform a morphological analysis of each galaxy. The asymmetry, concentration, and ellipticity of the dark burst hosts are compared against the host galaxies of optically bright GRBs. In agreement with other studies, we find that dark GRB hosts are redder and more luminous than the bulk of the GRB host population. The distribution of projected spatial offsets for dark GRBs from their host galaxy centroids is comparable to that of optically bright bursts. The dark GRB hosts are physically larger, more massive and redder, but are morphologically similar to the hosts of bright GRBs in terms of concentration and asymmetry. Our analysis constrains the fraction of high redshift (z &gt; 5) GRBs in the sample to 14 per cent, implying an upper limit for the whole long-GRB population of ≤4.4 per cent. If dust is the primary cause of afterglow darkening amongst dark GRBs, the measured extinction may require a clumpy dust component in order to explain the observed offset and ellipticity distributions.

scholarly journals The predicted properties of helium-enriched globular cluster progenitors at high redshift

2020 ◽  
Vol 496 (3) ◽  
pp. 3222-3234
Author(s):  
David M Nataf ◽  
Shunsaku Horiuchi ◽  
Guglielmo Costa ◽  
Rosemary F G Wyse ◽  
Yuan-Sen Ting ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Globular Cluster ◽  
Globular Clusters ◽  
Hubble Space Telescope ◽  
High Redshift ◽  
Cluster Formation ◽  
Stellar Populations ◽  
Space Telescope ◽  
James Webb Space Telescope ◽  
Galactic Astronomy

ABSTRACT Globular cluster progenitors may have been detected by Hubble Space Telescope, and are predicted to be observable with James Webb Space Telescope (JWST) and ground-based extremely large telescopes with adaptive optics. This has the potential to elucidate the issue of globular cluster formation and the origins of significantly helium-enriched subpopulations, a problem in Galactic astronomy with no satisfactory theoretical solution. Given this context, we use model stellar tracks and isochrones to investigate the predicted observational properties of helium-enriched stellar populations in globular cluster progenitors. We find that, relative to helium-normal populations, helium-enriched (ΔY = +0.12) stellar populations similar to those inferred in the most massive globular clusters, are expected, modulo some rapid fluctuations in the first ∼30 Myr, to be brighter and redder in the rest frame. At fixed age, stellar mass, and metallicity, a helium-enriched population is predicted to converge to being ∼0.40 mag brighter at $\lambda \approx 2.0\, {\mu \rm m}$, and to be 0.30-mag redder in the JWST–NIRCam colour (F070W − F200W), and to actually be fainter for $\lambda \lesssim 0.50 \, {\mu \rm m}$. Separately, we find that the time-integrated shift in ionizing radiation is a negligible $\sim \!5{{\ \rm per\ cent}}$, though we show that the Lyman-α escape fraction could end up higher for helium-enriched stars.

scholarly journals Ultraviolet spectropolarimetry of high-redshift quasars with the Hubble Space Telescope

1995 ◽  
Vol 440 ◽  
pp. 80 ◽  
Author(s):  
C. D. Impey ◽  
Matthew A. Malkan ◽  
Wayne Webb ◽  
C. E. Petry
Keyword(s):  
Hubble Space Telescope ◽  
High Redshift ◽  
Space Telescope

scholarly journals On the possibility of baryon acoustic oscillation measurements at redshift z > 7.6 with the Roman space telescope

2020 ◽  
Vol 498 (4) ◽  
pp. 4955-4970
Author(s):  
Siddharth Satpathy ◽  
Zhaozhou An ◽  
Rupert A C Croft ◽  
Tiziana Di Matteo ◽  
Ananth Tenneti ◽  
...  
Keyword(s):  
Large Scale ◽  
High Redshift ◽  
High Sensitivity ◽  
Acoustic Oscillation ◽  
Detection Sensitivity ◽  
Angular Diameter ◽  
Acoustic Oscillations ◽  
Space Telescope ◽  
Angular Diameter Distance ◽  
High Redshift Universe

ABSTRACT The Nancy Grace Roman Space Telescope (RST), with its field of view and high sensitivity will make surveys of cosmological large-scale structure possible at high redshifts. We investigate the possibility of detecting baryon acoustic oscillations (BAO) at redshifts z &gt; 7.6 for use as a standard ruler. We use data from the hydrodynamic simulation bluetides in conjunction with the gigaparsec-scale Outer Rim simulation and a model for patchy reionization to create mock RST High Latitude Survey grism data for Lyman α emission line selected galaxies at redshifts z = 7.4 to z = 10, covering 2280 deg2. We measure the monopoles of galaxies in the mock catalogues and fit the BAO features. We find that for a line flux of $L = 7\times 10^{-17} \ {\rm erg\, s^{-1}\, cm}^{-2}$, the 5σ detection limit for the current design, the BAO feature is partially detectable (measured in three out of four survey quadrants analysed independently). The resulting root mean square error on the angular diameter distance to z = 7.7 is 7.9 ${{\ \rm per\ cent}}$. If we improve the detection sensitivity by a factor of two (i.e. $L = 3.5\times 10^{-17} \ {\rm erg\, s^{-1}\, cm}^{-2}$), the distance error reduces to $1.4{{\ \rm per\ cent}}$. We caution that many more factors are yet to be modelled, including dust obscuration, the damping wing due to the intergalactic medium, and low redshift interlopers. If these issues do not strongly affect the results, or different observational techniques (such as use of multiple lines) can mitigate them, RST, or similar instruments may be able to constrain the angular diameter distance to the high redshift universe.

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