Day 752

Friday.
1409.7084
The Next Generation BLAST experiment
Galityki et al

BLASTPol was a suborbital experiment designed to map B fields in order to study their role in SF processes.  BLASTPol made detailed polarization maps of a number of molecular clouds during its successful flights from Antarctica in 2010 and 2012.  Present the next-generation BLASTPol instrument (BOAST-TNG) that will build off the success of the previous experiment and continue its role as a unique instrument and a test bed for new technologies.  With a 16-fold increase in mapping speed, BLAST-TNG will make larger and deeper maps.  Major improvements include a 2.5m carbon fiber mirror that is 40% wider that the BLASTPol mirror and ~3000 polarization sensitive detectors.  BLAST-TNG will observe in 3 bands at 250, 350, and 500 um.  The telescope will surge as a pathfinder project for microwave kinetic inductance detector (MKID) technology, as applied to feed horn coupled sub millimeter detector arrays.  The liquid He cooled cryostat will have a 28-day hold time and will utilize a closed-cycle 3He refrigerator to cool the detector arrays to 270 mK.  This will enable a detailed mapping of more targets with higher polarization resolution than any other sub millimeter experiment to date.  BLAST-TNG will also be the first balloon-borne telescope to offer shared risk observing time to the community.  This paper outlines the motivation for the project and the instrumental design.

1409.7119
CANDELS/GOODS-S, CDFS, ECDEF: Photometric redshifts for normal and for X-ray-detected galaxies
Hsu et al

Photo-z and PDF for all sources in ECDFS, finding 1207 counterparts to the 1259 X-ray sources.  Data used for photo-z include intermediate-band photometry deblended using the TFIT method, which is used for the first time in this work.  Photo-z for X-ray source counterparts are based on a new library of AGN/galaxy hybrid templates appropriate for the faint X-ray population in the CDFS.  Photo-z accuracy for normal galaxies is 0.010 and for X-ray sources is 0.014, and outlier fractions are 4% and 5.4% respectively.  The results within the CANDELS coverage area are even better as demonstrated both by spectroscopic comparison and by galaxy-pair statistics.  Intermediate-band photometry, even if shallow, is valuable when combined with deep broad-band photometry.  For best accuracy, templates must include emission lines.

1409.7245
How to determine an exomoon's sense of orbital motion
Heller, Albrecht

Present two methods to determine an exomoon's sense of orbital motion (SOM), one respect to the planet's circumstellar orbit and one with respect to the planetary rotation.  Simulations show E-ELT will be able to make these measurements.  The first method relies on the mutual planet-moon events during stellar transits.  Eclipses with the moon passing behind (in front of) the planet will be late (early) with regard to the moon's mean orbital period due to the finite speed of light.  This "transit timing dichotomy" (TTD) determines an exomoon's SOM with respect to the circumstellar motion.  For the ten largest moons in the solar system, TTDs range between 2 and 12 s.  the E-ELT will enable such measurements for Earth-sized moons around nearby stars.  The second method measures distortions in the IR spectrum of the rotation giant planet when it is transited by its moon.  This Rossiter-McLaughlin effect (RME) in the planetary spectrum reveals the angle between the planetary equator and the moon's curcumplanetary orbital plane, and therefore unveils the moon's SOM with respect to the planet's rotation.  A reasonably large moon transiting a directly imaged planet like beta Pic b cases an RME amplitude of almost 100 m/s, about twice the stellar RME amplitude of the transiting exoplanet HD209458b.  Both new methods can be used to probe the origin of exomoons, that is, whether they are regular or irregular in nature.

1409.7295
Galaxy and mass assembly (GAMA): the unimodal nature of the dwarf galaxy population
Mahajan et al

Obtain light profile of 432 galaxies, multi-band photometry in 18 broad bands to obtain M*, SFR, sSFR and M_dust.  Show that visually distinct, SF dwarf galaxies (irregulars, blue spheroids and low surface brightness galaxies) form a unimodal population in a parameter space mapped by mu_e, mu_0, n, r_e, SFR, sSFR, M*, M_dust and (g-i).  The SFR and sSFR distribution of passively evolving (dwarf) ellipticals on the other hand, statistically distinguish them from other galaxies with similar luminosity, while the giant galaxies clearly segregate into SF spirals and passive lenticulars.  Therefore suggest that the morphology classification scheme(s) used in the literature for dwarf galaxies only reflect the observational differences based on luminosity and surface brightness among the apparent distinct classes, rather than any physical differences between them.

1409.7297
Intrinsic alignments of galaxies in the MassiveBlack-II simulation: analysis of two-point statistics
Tenneti, Singh, Mandelbaum, et al

Present detailed measurements of the galaxy intrinsic alignments and associated ellipticity-direction (ED) and projected shape (w_g+) correlation functions for galaxies in the cosmological hydro MB-II simulation.  Carefully asses the effects on galaxy shapes, misalignments and 2-pt statistics of iterative weighted (by mass, luminosity, and color) definition of the (reduced and unreduced) inertia tensor.  Find that iterative procedures must be adopted for a reliable measurement of reduced tensor but that luminosity versus mass weighting has only negligible effects.  Blue galaxies exhibit stronger misalignments and suppressed w_g+ amplitude.  Both ED and w_g+ correlations increase in amplitude with sub halo mass (in the rage of 1e10-6e14 Msun/h), with a weak redshift dependence (from z=1 to z=0.06) at fixed mass.  At z~0.3, predict a w_g+ that is in reasonable agreement with SDSS LRG measurements and that decreases in amplitude by a factor of ~5-18 for galaxies in the LSST survey.  Predict the ratio of w_g+ (using sub haloes as tracers of density) and w_delta+ (using DM density) to exhibit a scale dependent bias on scales where the 1-halo term dominates.  Also compared the IA of centrals and satellites, with clear detection of satellite radial alignments within their host haloes.  Finally, show that w_g+ and w_delta+ predictions from the simulation agree with that of NL alignment models at scales where the 2-halo term dominates in the correlations (and tabulate associated NLA fitting parameters).