Day 919

Tuesday.


1507.00999
An empirical model for the galaxy luminosity and star-formation rate function at high redshift
Mashian, Oesch, Loeb

Using the most recent measurements of the UV LFs and dust estimates of early galaxies, derive updated dust-corrected SFR functions (SFRFs) at z~4-8, which are modeled to predict the evolution to higher redshifts, z>8.  Employ abundance matching techniques to calibrate a relation between galaxy SFR and host halo mass M_h by mapping the shape of the observed SFRFs at z~4-8 to that of the halo MF.  The resulting scaling law remains roughly constant over this z range.  Apply the average SFR-M_h relation to reproduce the observed SFR functions at 4<=z<=8 and also derive the expected UV LFs at higher redshifts.  At z~9 and ~10 these model LFs are in excellent agreement with current observed estimates.  The predicted number densities and UV LFs at z>10 indicate that JWST will be able to detect galaxies out to z~15 with an extensive treasury sized program.  Also derive the z evolution of the SFR density and associated reionization history by galaxies, where it is found that the inclusion of galaxies with SFRs well below the current detection limit leads to a fully recognized universe by z6.5 and an optical depth of tau~0.054, consistent with the recently derived Planck value at the 1 sigma level.


1507.01005
A three-dimensional map of Milky-Way dust
Green, Scholarly, FInkbeiner, Rix, ... et al

Present a 3-d map of interstellar dust reddening, covering 3/4 of the sky out to a distance of several kpc, based on Pan-STARRS1 and 2MASS photometry.  The map reveals a wealth of detailed structure, from filaments to large cloud complexes.  The map has a hybrid angular resolution, with most of the map at an angular resolution of 3.4' to 13.7', and a maximum distance resolution of ~25%.  The 3-d distribution of dust is determined in a fully probabilistic framework, yielding the uncertainty in the reddening distribution along each LoS, as well as stellar distances, reddenings and classifications for 800 M stars detected by PS1.  Demonstrate the consistency of the reddening estimates with those of 2D emission-based maps of dust reddening.  In particular, find agreement with the Planck 353 GHz optical depth-based reddening map to within 0.05 mag in E(B-V) to a depth of 0.5 mag, and explore systematics at reddenings less than E(B-V)~0.08 mag.  Validate the per-star reddening estimates by comparison with reddening estimates for stars with both SDSS photometry and SEGUE spectral classifications, finding per-star agreement to within 0.1 mag out to a stellar E(B-V) of 1 mag.  Compare the map to two existing 3-dimensional dust maps, by Marshall+2006 and Lallement+2013, demonstrating the finer resolution of this work, and better distance resolution compared to the former within ~3 kpc.  The map can be queried or downloaded at argonaut.skymaps.info.  Expect the 3D reddening map presented here to find a wide range of uses, among them correcting for reddening and extinction for objects embedded in the plane of the Galaxy, studies of Galactic structure, calibration of future emission-based dust maps and determining distances to objects of known reddening.


1507.01214
Early type galaxies and structural parameters from ESO public survey KiDS
Roy, Napolitano, ... et al

KiDS @ VST is an ideal tool for galaxy evolution studies.  Expect to observe millions of galaxies for which the structural parameters are extracted in ugr and i.  This sample will represent the largest dataset with measured structural parameters up to z=0.5.  In this paper, introduce the sample, and describe the 2D fitting procedure using the 2DPHOT environment and the validation of the parameters with an external catalog.  [Conference proceedings.]


1507.01464
Measuring subhalo mass in redMaPPer clusters with CFHT Strip 82 survey
Li, .. Kneib, Mo, Rozo, Leauthaud, ... et al

Use the shear catalog from the CFHT Stripe-82 survey to measure the sub halo masses of satellite galaixies in redMaPPer clusters.  Assuming a Chabrier IMF and a truncated NFW model for the sub halo mass distribution, find that the sub-halo mass to galaxy stellar mass ratio increases as a function of projected halo-centric radius r_p, from Msub/M*=3.5+4.5-2.5 at r_p in [0.1,0.3] Mpc/h to Msub/M*=41+12-12 at r_p in [0.6,0.8] Mpc/h.  Also investigate the dependence of sub halo masses on stellar mass by splitting satellite galaxies into two stellar mass bins: 10<log(M*/Ms)<10.75 and 1.75 .. 12.  The mean sub halo mass of the more massive satellite galaxy bin is about 5x largers than that of the less massive satellites: log(Msub/Ms)=12.1 (Msun/M*=12±5) vs log (Msun/Ms)=11.37(Msub/M*)=17±16.