ABSTRACT We present reduced data and data products from the 3D-HST survey, a 248-orbit HST Treasury program. The survey obtained WFC3 G141 grism spectroscopy in four of the five CANDELS fields: ...AEGIS, COSMOS, GOODS-S, and UDS, along with WFC3 H140 imaging, parallel ACS G800L spectroscopy, and parallel I814 imaging. In a previous paper, we presented photometric catalogs in these four fields and in GOODS-N, the fifth CANDELS field. Here we describe and present the WFC3 G141 spectroscopic data, again augmented with data from GO-1600 in GOODS-N (PI: B. Weiner). We developed software to automatically and optimally extract interlaced two-dimensional (2D) and one-dimensional (1D) spectra for all objects in the Skelton et al. (2014) photometric catalogs. The 2D spectra and the multi-band photometry were fit simultaneously to determine redshifts and emission line strengths, taking the morphology of the galaxies explicitly into account. The resulting catalog has redshifts and line strengths (where available) for 22,548 unique objects down to (79,609 unique objects down to ). Of these, 5459 galaxies are at and 9621 are at , where H falls in the G141 wavelength coverage. The typical redshift error for galaxies is , i.e., one native WFC3 pixel. The limit for emission line fluxes of point sources is erg s−1 cm−2. All 2D and 1D spectra, as well as redshifts, line fluxes, and other derived parameters, are publicly available.18
ABSTRACT
We present H
α
maps at 1 kpc spatial resolution for star-forming galaxies at
z
∼ 1, made possible by the Wide Field Camera 3 grism on
Hubble Space Telescope
(
HST
). Employing this ...capability over all five 3D-
HST
/CANDELS fields provides a sample of 3200 galaxies enabling a division into subsamples based on stellar mass and star formation rate (SFR). By creating deep stacked H
α
images, we reach surface brightness limits of 1 × 10
−18
erg s
−1
cm
−2
arcsec
−2
, allowing us to map the distribution of ionized gas to ∼10 kpc for typical
L
* galaxies at this epoch. We find that the spatial extent of the H
α
distribution increases with stellar mass as
kpc. The H
α
emission is more extended than the stellar continuum emission, consistent with inside-out assembly of galactic disks. This effect grows stronger with mass as
. We map the H
α
distribution as a function of SFR(IR+UV) and find evidence for “coherent star formation” across the SFR–
M
*
plane: above the main sequence (MS), H
α
is enhanced at all radii; below the MS, H
α
is depressed at all radii. This suggests that at all masses the physical processes driving the enhancement or suppression of star formation act throughout the disks of galaxies. At high masses (
), above the MS, H
α
is particularly enhanced in the center, potentially building bulges and/or supermassive black holes. Below the MS, a strong central dip in the EW(H
α
), as well as the inferred specific SFR, appears. Importantly, though, across the entirety of the SFR–
M
*
plane, the absolute SFR as traced by H
α
is always centrally peaked, even in galaxies below the MS.
Joint studies of imaging and spectroscopic samples, informed by theory and simulations, offer the potential for comprehensive tests of the cosmological model over redshifts z<1.5. Spectroscopic ...galaxy samples at these redshifts can be increased beyond the planned Dark Energy Spectroscopic Instrument (DESI) program by at least an order of magnitude, thus offering significantly more constraining power for these joint studies. Spectroscopic observations of these galaxies in the latter half of the 2020's and beyond would leverage the theory and simulation effort in this regime. In turn, these high density observations will allow enhanced tests of dark energy, physics beyond the standard model, and neutrino masses that will greatly exceed what is currently possible. Here, we present a coordinated program of simulations, theoretical modeling, and future spectroscopy that would enable precise cosmological studies in the accelerating epoch where the effects of dark energy are most apparent.
In this investigation, we leverage the combination of Dark Energy Spectroscopic Instrument Legacy imaging Surveys Data Release 9 (DESI LS DR9), Survey Validation 3 (SV3), and Year 1 (Y1) data sets to ...estimate the conditional luminosity and stellar mass functions (CLFs & CSMFs) of galaxies across various halo mass bins and redshift ranges. To support our analysis, we utilize a realistic DESI Mock Galaxy Redshift Survey (MGRS) generated from a high-resolution Jiutian simulation. An extended halo-based group finder is applied to both MGRS catalogs and DESI observation. By comparing the r and z-band luminosity functions (LFs) and stellar mass functions (SMFs) derived using both photometric and spectroscopic data, we quantified the impact of photometric redshift (photo-z) errors on the galaxy LFs and SMFs, especially in the low redshift bin at low luminosity/mass end. By conducting prior evaluations of the group finder using MGRS, we successfully obtain a set of CLF and CSMF measurements from observational data. We find that at low redshift the faint end slopes of CLFs and CSMFs below \(10^{9}h^{-2}L_{\odot}\) (or \(h^{-2}M_{\odot}\)) evince a compelling concordance with the subhalo mass functions. After correcting the cosmic variance effect of our local Universe following arXiv:1809.00523, the faint end slopes of the LFs/SMFs turn out to be also in good agreement with the slope of the halo mass function.
The joint analysis of different cosmological probes, such as galaxy clustering and weak lensing, can potentially yield invaluable insights into the nature of the primordial Universe, dark energy and ...dark matter. However, the development of high-fidelity theoretical models that cover a wide range of scales and redshifts is a necessary stepping-stone. Here, we present public high-resolution weak lensing maps on the light cone, generated using the \(N\)-body simulation suite AbacusSummit in the Born approximation, and accompanying weak lensing mock catalogues, tuned via fits to the Early Data Release small-scale clustering measurements of the Dark Energy Spectroscopic Instrument (DESI). Available in this release are maps of the cosmic shear, deflection angle and convergence fields at source redshifts ranging from \(z = 0.15\) to 2.45 with \(\Delta z = 0.05\) as well as CMB convergence maps (\(z \approx 1090\)) for each of the 25 \({\tt base}\)-resolution simulations (\(L_{\rm box} = 2000\,h^{-1}{\rm Mpc}\), \(N_{\rm part} = 6912^3\)) as well as for the two \({\tt huge}\) simulations (\(L_{\rm box} = 7500\,h^{-1}{\rm Mpc}\), \(N_{\rm part} = 8640^3\)) at the fiducial AbacusSummit cosmology (\(Planck\) 2018). The pixel resolution of each map is 0.21 arcmin, corresponding to a HEALPiX \(N_{\rm side}\) of 16384. The sky coverage of the \({\tt base}\) simulations is an octant until \(z \approx 0.8\) (decreasing to about 1800 deg\(^2\) at \(z \approx 2.4\)), whereas the \({\tt huge}\) simulations offer full-sky coverage until \(z \approx 2.2\). Mock lensing source catalogues are sampled matching the ensemble properties of the Kilo-Degree Survey, Dark Energy Survey, and Hyper-Suprime Cam weak lensing datasets. The produced mock catalogues are validated against theoretical predictions for various clustering and lensing statistics such as galaxy clustering multipoles, galaxy-shear and shear-shear, showing excellent agreement.
The canonical cosmological model, the Lambda Cold Dark Matter (ΛCDM) model, postulates that around 95% of the Universe consists of dark energy and Cold Dark Matter (CDM). Despite the unknown physical ...nature of these forms of matter and energy, the ΛCDM model provides accurate predictions for a variety of observations. One of the main pillars of cosmology is the large-scale distribution of galaxies as probed by galaxy surveys like the Sloan Digital Sky Survey (SDSS). The ultimate goal of this dissertation is to improve and apply methods to test the ΛCDM cosmological paradigm with current and future galaxy surveys. A particular focus of this work is probing the cosmological paradigm with the matter and galaxy distribution on small, so-called non-linear scales. Among the most fundamental non-linear structures in cosmology are gravitationally collapsed, virialized dark matter halos. These halos provide the gravitational potential well for gas to condense and crystallize into galaxies. Studying the small-scale distribution of matter and galaxies thus requires a detailed characterization of the relationship between galaxies and dark matter halos, the galaxy-halo connection. Additionally, using non-linear scales comes with a plethora of additional challenges compared to large, so-called linear scales. However, non-linear scales have the strongest statistical constraining power, thus providing the largest potential insight into the galaxy-halo connection and cosmology. Therefore, this work is aimed at making measurements on non-linear scales a robust testbed for theories of galaxy formation and cosmology. In detail, the topics covered in this dissertation are as follows: this work analyzes how often the brightest galaxies in a dark matter halo are located in the halo center in the SDSS. Additionally, a theoretical study of how the motions of satellite galaxies can be used to study the galaxy-halo connection is presented. Furthermore, this updated method based on the kinematics of satellite galaxies is then applied to the SDSS and its implications for galaxy formation discussed. Moreover, the small-scale clustering and galaxy-galaxy lensing signal of galaxies in the Baryon Oscillation Spectroscopic Survey (BOSS) is analyzed, as well as its implications for the ΛCDM paradigm and the galaxy-halo connection examined. Finally, a new, highly accurate statistical framework for studying cosmology with small-scale galaxy and matter distributions is discussed and demonstrated.
ABSTRACT We present H maps at 1 kpc spatial resolution for star-forming galaxies at z ∼ 1, made possible by the Wide Field Camera 3 grism on Hubble Space Telescope (HST). Employing this capability ...over all five 3D-HST/CANDELS fields provides a sample of 3200 galaxies enabling a division into subsamples based on stellar mass and star formation rate (SFR). By creating deep stacked H images, we reach surface brightness limits of 1 × 10−18 erg s−1 cm−2 arcsec−2, allowing us to map the distribution of ionized gas to ∼10 kpc for typical L* galaxies at this epoch. We find that the spatial extent of the H distribution increases with stellar mass as kpc. The H emission is more extended than the stellar continuum emission, consistent with inside-out assembly of galactic disks. This effect grows stronger with mass as . We map the H distribution as a function of SFR(IR+UV) and find evidence for "coherent star formation" across the SFR-M* plane: above the main sequence (MS), H is enhanced at all radii; below the MS, H is depressed at all radii. This suggests that at all masses the physical processes driving the enhancement or suppression of star formation act throughout the disks of galaxies. At high masses ( ), above the MS, H is particularly enhanced in the center, potentially building bulges and/or supermassive black holes. Below the MS, a strong central dip in the EW(H ), as well as the inferred specific SFR, appears. Importantly, though, across the entirety of the SFR-M* plane, the absolute SFR as traced by H is always centrally peaked, even in galaxies below the MS.
We present Ha maps at 1kpc spatial resolution for star-forming galaxies at z~1, made possible by the WFC3 grism on HST. Employing this capability over all five 3D-HST/CANDELS fields provides a sample ...of 2676 galaxies. By creating deep stacked Halpha (Ha) images, we reach surface brightness limits of 1x10^-18\erg\s\cm^2\arcsec^2, allowing us to map the distribution of ionized gas out to >10kpc for typical L* galaxies at this epoch. We find that the spatial extent of the Ha distribution increases with stellar mass as r(Ha)kpc=1.5(Mstars/10^10Msun)^0.23. Furthermore, the Ha emission is more extended than the stellar continuum emission, consistent with inside-out assembly of galactic disks. This effect, however, is mass dependent with r(Ha)/r(stars)=1.1(M/10^10Msun)^0.054, such that at low masses r(Ha)~r(stars). We map the Ha distribution as a function of SFR(IR+UV) and find evidence for `coherent star formation' across the SFR-M plane: above the main sequence, Ha is enhanced at all radii; below the main sequence, Ha is depressed at all radii. This suggests that at all masses the physical processes driving the enhancement or suppression of star formation act throughout the disks of galaxies. It also confirms that the scatter in the star forming main sequence is real and caused by variations in the star formation rate at fixed mass. At high masses (10^10.5<M/Msun<10^11), above the main sequence, Ha is particularly enhanced in the center, plausibly building bulges and/or supermassive black holes. Below the main sequence, the star forming disks are more compact and a strong central dip in the EW(Ha), and the inferred specific star formation rate, appears. Importantly though, across the entirety of the SFR-M plane, the absolute star formation rate as traced by Ha is always centrally peaked, even in galaxies below the main sequence.
We present reduced data and data products from the 3D-HST survey, a 248-orbit
HST Treasury program. The survey obtained WFC3 G141 grism spectroscopy in four
of the five CANDELS fields: AEGIS, COSMOS, ...GOODS-S, and UDS, along with WFC3
$H_{140}$ imaging, parallel ACS G800L spectroscopy, and parallel $I_{814}$
imaging. In a previous paper (Skelton et al. 2014) we presented photometric
catalogs in these four fields and in GOODS-N, the fifth CANDELS field. Here we
describe and present the WFC3 G141 spectroscopic data, again augmented with
data from GO-1600 in GOODS-N. The data analysis is complicated by the fact that
no slits are used: all objects in the WFC3 field are dispersed, and many
spectra overlap. We developed software to automatically and optimally extract
interlaced 2D and 1D spectra for all objects in the Skelton et al. (2014)
photometric catalogs. The 2D spectra and the multi-band photometry were fit
simultaneously to determine redshifts and emission line strengths, taking the
morphology of the galaxies explicitly into account. The resulting catalog has
98,663 measured redshifts and line strengths down to $JH_{IR}\leq 26$ and
22,548 with $JH_{IR}\leq 24$, where we comfortably detect continuum emission.
Of this sample 5,459 galaxies are at $z>1.5$ and 9,621 are at $0.7<z<1.5$,
where H$\alpha$ falls in the G141 wavelength coverage. Based on comparisons
with ground-based spectroscopic redshifts, and on analyses of paired galaxies
and repeat observations, the typical redshift error for $JH_{IR}\leq 24$
galaxies in our catalog is $\sigma_z \approx 0.003 \times (1+z)$, i.e., one
native WFC3 pixel. The $3\sigma$ limit for emission line fluxes of point
sources is $1.5\times10^{-17}$ ergs s$^{-1}$ cm$^{-2}$. We show various
representations of the full dataset, as well as individual examples that
highlight the range of spectra that we find in the survey.
We present reduced data and data products from the 3D-HST survey, a 248-orbit HST Treasury program. The survey obtained WFC3 G141 grism spectroscopy in four of the five CANDELS fields: AEGIS, COSMOS, ...GOODS-S, and UDS, along with WFC3 \(H_{140}\) imaging, parallel ACS G800L spectroscopy, and parallel \(I_{814}\) imaging. In a previous paper (Skelton et al. 2014) we presented photometric catalogs in these four fields and in GOODS-N, the fifth CANDELS field. Here we describe and present the WFC3 G141 spectroscopic data, again augmented with data from GO-1600 in GOODS-N. The data analysis is complicated by the fact that no slits are used: all objects in the WFC3 field are dispersed, and many spectra overlap. We developed software to automatically and optimally extract interlaced 2D and 1D spectra for all objects in the Skelton et al. (2014) photometric catalogs. The 2D spectra and the multi-band photometry were fit simultaneously to determine redshifts and emission line strengths, taking the morphology of the galaxies explicitly into account. The resulting catalog has 98,663 measured redshifts and line strengths down to \(JH_{IR}\leq 26\) and 22,548 with \(JH_{IR}\leq 24\), where we comfortably detect continuum emission. Of this sample 5,459 galaxies are at \(z>1.5\) and 9,621 are at \(0.7<z<1.5\), where H\(\alpha\) falls in the G141 wavelength coverage. Based on comparisons with ground-based spectroscopic redshifts, and on analyses of paired galaxies and repeat observations, the typical redshift error for \(JH_{IR}\leq 24\) galaxies in our catalog is \(\sigma_z \approx 0.003 \times (1+z)\), i.e., one native WFC3 pixel. The \(3\sigma\) limit for emission line fluxes of point sources is \(1.5\times10^{-17}\) ergs s\(^{-1}\) cm\(^{-2}\). We show various representations of the full dataset, as well as individual examples that highlight the range of spectra that we find in the survey.
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