اشترك بالحزمة الذهبية واحصل على وصول غير محدود شمرا أكاديميا
تسجيل مستخدم جديدHubble Frontier Fields First Complete Cluster Data: Faint Galaxies at $zsim 5-10$ for UV Luminosity Functions and Cosmic Reionization
117
0
0.0
(
0
)
اسأل ChatGPT حول البحث
ﻻ يوجد ملخص باللغة العربية
We present the comprehensive analyses of faint dropout galaxies up to $zsim10$ with the first full-depth data set of Abell 2744 lensing cluster and parallel fields observed by the Hubble Frontier Fields (HFF) program. We identify $54$ dropouts at $zsim5-10$ in the HFF fields, and enlarge the size of $zsim9$ galaxy sample obtained to date. Although the number of highly magnified ($musim10$) galaxies is small due to the tiny survey volume of strong lensing, our study reaches the galaxies intrinsic luminosities comparable to the deepest-field HUDF studies. We derive UV luminosity functions with these faint dropouts, carefully evaluating the combination of observational incompleteness and lensing effects in the image plane by intensive simulations including magnification, distortion, and multiplication of images, with the evaluations of mass model dependences. Our results confirm that the faint-end slope, $alpha$, is as steep as $-2$ at $zsim6-8$, and strengthen the evidence of the rapid decrease of UV luminosity densities, $rho_mathrm{UV}$, at $z>8$ from the large $zsim9$ sample. We examine whether the rapid $rho_mathrm{UV}$ decrease trend can reconcile with the large Thomson scattering optical depth, $tau_mathrm{e}$, measured by CMB experiments allowing a large space of free parameters such as average ionizing photon escape fraction and stellar-population dependent conversion factor. No parameter set can reproduce both the rapid $rho_mathrm{UV}$ decrease and the large $tau_mathrm{e}$. It is possible that the $rho_mathrm{UV}$ decrease moderates at $zgtrsim11$, that the free parameters significantly evolve towards high-$z$, or that there exist additional sources of reionization such as X-ray binaries and faint AGNs.
قيم البحث
اقرأ أيضاً
We present UV luminosity functions of dropout galaxies at $zsim6-10$ with the complete Hubble Frontier Fields data. We obtain a catalog of $sim450$ dropout-galaxy candidates (350, 66, and 40 at $zsim6-7$, 8, and 9, respectively), whose UV absolute ma
gnitudes reach $sim-14$ mag, $sim2$ mag deeper than the Hubble Ultra Deep Field detection limits. We carefully evaluate number densities of the dropout galaxies by Monte-Carlo simulations, including all lensing effects such as magnification, distortion, and multiplication of images as well as detection completeness and contamination effects in a self-consistent manner. We find that UV luminosity functions at $zsim6-8$ have steep faint-end slopes, $alphasim-2$, and likely steeper slopes, $alphalesssim-2$ at $zsim9-10$. We also find that the evolution of UV luminosity densities shows a non-accelerated decline beyond $zsim8$ in the case of $M_mathrm{trunc}=-15$, while an accelerated in the case of $M_mathrm{trunc}=-17$. We examine whether our results are consistent with the Thomson scattering optical depth from the Planck satellite and the ionized hydrogen fraction $Q_mathrm{HII}$ at $zlesssim7$ based on the standard analytic reionization model. We find that there exist reionizaiton scenarios that consistently explain all the observational measurements with the allowed parameters of $f_{rm esc}=0.17^{+0.07}_{-0.03}$ and $M_mathrm{trunc}>-14.0$ for $logxi_mathrm{ion}/[mathrm{erg}^{-1} mathrm{Hz}]=25.34$, where $f_{rm esc}$ is the escape fraction, $M_mathrm{trunc}$ is the faint limit of the UV luminosity function, and $xi_mathrm{ion}$ is the conversion factor of the UV luminosity to the ionizing photon emission rate. The length of the reionization period is estimated to be $Delta z=3.9^{+2.0}_{-1.6}$ (for $0.1<Q_mathrm{HII}<0.99$), consistent with the recent estimate from Planck.
We present the results of a new search for galaxies at redshift z ~ 9 in the first two Hubble Frontier Fields with completed HST WFC3/IR and ACS imaging. To ensure robust photometric redshift solutions, and to minimize incompleteness, we confine our
search to objects with H_{160} < 28.6 (AB mag), consider only image regions with an rms noise sigma_{160} > 30 mag (within a 0.5-arcsec diameter aperture), and insist on detections in both H_{160} and J_{140}. The result is a survey covering an effective area (after accounting for magnification) of 10.9 sq. arcmin, which yields 12 galaxies at 8.4 < z < 9.5. Within the Abell-2744 cluster and parallel fields we confirm the three brightest objects reported by Ishigaki et al. (2014), but recover only one of the four z > 8.4 sources reported by Zheng et al. (2014). In the MACSJ0416.1-240 cluster field we report five objects, and explain why each of these eluded detection or classification as z ~ 9 galaxies in the published searches of the shallower CLASH data. Finally, we uncover four z ~ 9 galaxies from the previously unsearched MACSJ0416.1-240 parallel field. Based on the published magnification maps we find that only one of these 12 galaxies is likely boosted by more than a factor of two by gravitational lensing. Consequently we are able to perform a fairly straightforward reanalysis of the normalization of the z ~ 9 UV galaxy luminosity function as explored previously in the HUDF12 programme. We conclude that the new data strengthen the evidence for a continued smooth decline in UV luminosity density (and hence star-formation rate density) from z ~ 8 to z ~ 9, contrary to recent reports of a marked drop-off at these redshifts. This provides further support for the scenario in which early galaxy evolution is sufficiently extended to explain cosmic reionization.
We measure the size-mass relation and its evolution between redshifts 1$<z<$3, using galaxies lensed by six foreground Hubble Frontier Fields clusters. The power afforded by strong gravitation lensing allows us to observe galaxies with higher angular
resolution beyond current facilities. We select a stellar mass limited sample and divide them into star-forming or quiescent classes based on their rest-frame UVJ colors from the ASTRODEEP catalogs. Source reconstruction is carried out with the recently-released $lenstruction$ software, which is built on the multi-purpose gravitational lensing software $lenstronomy$. We derive the empirical relation between size and mass for the late-type galaxies with $M_{*}>3times10^{9}M_{odot}$ at 1$<z<$2.5 and $M_* >5 times 10^{9} M_{odot}$ at 2.5$<z<$3, and at a fixed stellar mass, we find galaxy sizes evolve as $R_{eff}propto (1+z)^{-1.05pm0.37}$. The intrinsic scatter is $<0.1$ dex at $z<1.5$ but increases to $sim0.3$ dex at higher redshift. The results are in good agreement with those obtained in blank fields. We evaluate the uncertainties associated with the choice of lens model by comparing size measurements using five different and publicly available models, finding the choice of lens model leads to a 3.7 % uncertainty of the median value, and $sim 25$ % scatter for individual galaxies. Our work demonstrates the use of strong lensing magnification to boost resolution does not introduce significant uncertainties in this kind of work, and paves the way for wholesale applications of the sophisticated lens reconstruction technique to higher redshifts and larger samples.
The remarkable HST datasets from the CANDELS, HUDF09, HUDF12, ERS, and BoRG/HIPPIES programs have allowed us to map out the evolution of the UV LF from z~10 to z~4. We have identified 5859, 3001, 857, 481, 217, and 6 galaxy candidates at z~4, z~5, z~
6, z~7, z~8, and z~10, respectively from the ~1000 arcmin**2 area probed. The selection of z~4-8 galaxies over the five CANDELS fields allows us to assess the cosmic variance; the largest variations are apparent at z>=7. Our new LF determinations at z~4 and z~5 span a 6-mag baseline (-22.5 to -16 AB mag). These determinations agree well with previous estimates, but the larger samples and volumes probed here result in a more reliable sampling of >L* galaxies and allow us to reassess the form of the UV LFs. Our new LF results strengthen our earlier findings to 3.4 sigma significance for a steeper faint-end slope to the UV LF at z>4, with alpha evolving from alpha=-1.64+/-0.04 at z~4 to alpha=-2.06+/-0.13 at z~7 (and alpha = -2.02+/-0.23 at z~8), consistent with that expected from the evolution of the halo mass function. With our improved constraints at the bright end, we find less evolution in the characteristic luminosity M* over the redshift range z~4 to z~7; the observed evolution in the LF is now largely represented by changes in phi*. No evidence for a non-Schechter-like form to the z~4-8 LFs is found. A simple conditional LF model based on halo growth and evolution in the M/L ratio of halos ((1+z)**-1.5) provides a good representation of the observed evolution.
Ultra-faint galaxies are hosted by small dark matter halos with shallow gravitational potential wells, hence their star formation activity is more sensitive to feedback effects. The shape of the faint-end of the high-$z$ galaxy luminosity function (L
F) contains important information on star formation and its interaction with the reionization process during the Epoch of Reionization (EoR). High-$z$ galaxies with $M_{rm UV}gtrsim-17$ have only recently become accessible thanks to the Frontier Fields (FFs) survey combining deep {it HST} imaging and the gravitational lensing effect. In this paper we investigate the faint-end of the LF at redshift $>$5 using the data of FFs clusters Abell 2744 (A2744), MACSJ0416.1-2403 (M0416), MACSJ0717.5+3745 (M0717) and MACSJ1149.5+2223 (M1149). We analyze both an empirical and a physically-motivated LF model to obtain constraints on a possible turn-over of LF at faint magnitudes. In the empirical model the LF drops fast when the absolute UV magnitude $M_{rm UV}$ is much larger than a turn-over absolute UV magnitude $M_{rm UV}^{rm T}$. We obtain $M_{rm UV}^{rm T}gtrsim-14.6 $ (15.2) at 1 (2) $sigma$ confidence level (C.L.) for $zsim6$. In the physically-motivated analytical model, star formation in halos with circular velocity below $v_c^*$ is fully quenched if these halos are located in ionized regions. Using updated lensing models and new additional FFs data, we re-analyze previous constraints on $v_c^*$ and $f_{rm esc}$ presented by Castellano et al. 2016a (C16a) using a smaller dataset. We obtain new constraints on $v_c^*lesssim 59$ km s$^{-1}$ and $f_{rm esc}lesssim 56%$ (both at 2$sigma$ C.L.) and conclude that there is no turn-over detected so far from the analyzed FFs data. Forthcoming {it JWST} observations will be key to tight these constraints further.
سجل دخول لتتمكن من نشر تعليقات
التعليقات
جاري جلب التعليقات
سجل دخول لتتمكن من متابعة معايير البحث التي قمت باختيارها
