282 research outputs found
A constant limiting mass scale for flat early-type galaxies from z=1 to z=0: density evolves but shapes do not
We measure the evolution in the intrinsic shape distribution of early-type
galaxies from z~1 to z~0 by analyzing their projected axis-ratio distributions.
We extract a low-redshift sample (0.04 < z < 0.08) of early-type galaxies with
very low star-formation rates from the SDSS, based on a color-color selection
scheme and verified through the absence of emission lines in the spectra. The
inferred intrinsic shape distribution of these early-type galaxies is strongly
mass dependent: the typical short-to-long intrinsic axis-ratio of high-mass
early-type galaxies (>1e11 M_sun) is 2:3, where as at masses below 1e11 M_sun
this ratio narrows to 1:3, or more flattened galaxies. In an entirely analogous
manner we select a high-redshift sample (0.6 < z < 0.8) from two deep-field
surveys: GEMS and COSMOS. We find a seemingly universal mass of ~1e11 M_sun for
highly flatted early-type systems at all redshifts. This implies that the
process that grows an early-type galaxy above this ceiling mass involves
forming round systems. Using both parametric and non-parametric tests, we find
no evolution in the projected axis-ratio distribution for galaxies with masses
>3e10 M_sun with redshift. At the same time, our samples imply an increase of
2-3x in co-moving number density for early-type galaxies at masses >3e10 M_sun,
in agreement with previous studies. Given the direct connection between the
axis-ratio distribution and the underlying bulge-to-disk ratio distribution,
our findings imply that the number density evolution of early-type galaxies is
not exclusively driven by the emergence of either bulge- or disk-dominated
galaxies, but rather by a balanced mix that depends only on the stellar mass of
the galaxy. The challenge for galaxy formation models is to reproduce this
overall non-evolving ratio of flattened to round early-type galaxies in the
context of a continually growing population.Comment: 14 pages in emulate ApJ format, 8 color figures, submitted to ApJ,
comments welcome, fixed missing reference
Stellar and Gaseous Nuclear Disks Observed in Nearby (U)LIRGs
We present near-infrared integral field spectroscopy of the central
kiloparsec of 17 nearby luminous and ultra-luminous infrared galaxies
undergoing major mergers. These observations were taken with OSIRIS assisted by
the Keck I and II Adaptive Optics systems, providing spatial resolutions of a
few tens of parsecs. The resulting kinematic maps reveal gas disks in at least
16 out of 19 nuclei and stellar disks in 11 out of 11 nuclei observed in these
galaxy merger systems. In our late-stages mergers, these disks are young
(stellar ages Myr) and likely formed as gas disks which became unstable
to star formation during the merger. On average, these disks have effective
radii of a few hundred parsecs, masses between and ,
and between 1 and 5. These disks are similar to those created in
high-resolution hydrodynamical simulations of gas-rich galaxy mergers, and
favor short coalescence times for binary black holes. The few galaxies in our
sample in earlier stages of mergers have disks which are larger
( pc) and likely are remnants of the galactic disks that
have not yet been completely disrupted by the merger.Comment: accepted for publication in Ap
The Detection of Intergalactic Halpha Emission from the Slug Nebula at z~2.3
The Slug Nebula is one of the largest and most luminous Lyman-alpha (LyA)
nebulae discovered to date, extending over 450 kiloparsecs (kpc) around the
bright quasar UM287 at z=2.283. Characterized by high surface brightnesses over
intergalactic scales, its LyA emission may either trace high-density ionized
gas ("clumps") or large column densities of neutral material. To distinguish
between these two possibilities, information from a non-resonant line such as
Halpha is crucial. Therefore, we analyzed a deep MOSFIRE observation of one of
the brightest LyA emitting regions in the Slug Nebula with the goal of
detecting associated Halpha emission. We also obtained a deep, moderate
resolution LyA spectrum of the nearby brightest region of the Slug. We detected
an Halpha flux of F_(Halpha)= 2.62 +/- 0.47 x 10^-17 erg/cm^2/s
(SB_(Halpha)=2.70 +/- 0.48 x 10^-18 erg/cm^2/s/sq") at the expected spatial and
spectral location. Combining the Halpha detection with its corresponding LyA
flux (determined from the narrow-band imaging) we calculate a flux ratio of
F_(LyA_/F_(Halpha)= 5.5 +/- 1.1. The presence of a skyline at the location of
the Halpha emission decreases the signal to noise ratio of the detection and
our ability to put stringent constraints on the Halpha kinematics. Our
measurements argue for the origin of the LyA emission being recombination
radiation, suggesting the presence of high-density ionized gas. Finally, our
high-resolution spectroscopic study of the LyA emission does not show evidence
of a rotating disk pattern and suggest a more complex origin for at least some
parts of the Slug Nebula.Comment: 17 pages, 9 figures, final version including referee's comments after
acceptanc
The Dependence of Star Formation Rates on Stellar Mass and Environment at z~0.8
We examine the star formation rates (SFRs) of galaxies in a redshift slice
encompassing the z=0.834 cluster RX J0152.7-1357. We used a low-dispersion
prism in the Inamori Magellan Areal Camera and Spectrograph (IMACS) to identify
galaxies with z<23.3 AB mag in diverse environments around the cluster out to
projected distances of ~8 Mpc from the cluster center. We utilize a
mass-limited sample (M>2x10^{10} M_sun) of 330 galaxies that were imaged by
Spitzer MIPS at 24 micron to derive SFRs and study the dependence of specific
SFR (SSFR) on stellar mass and environment. We find that the SFR and SSFR show
a strong decrease with increasing local density, similar to the relation at
z~0. Our result contrasts with other work at z~1 that find the SFR-density
trend to reverse for luminosity-limited samples. These other results appear to
be driven by star-formation in lower mass systems (M~10^{10} M_sun). Our
results imply that the processes that shut down star-formation are present in
groups and other dense regions in the field. Our data also suggest that the
lower SFRs of galaxies in higher density environments may reflect a change in
the ratio of star-forming to non-star-forming galaxies, rather than a change in
SFRs. As a consequence, the SFRs of star-forming galaxies, in environments
ranging from small groups to clusters, appear to be similar and largely
unaffected by the local processes that truncate star-formation at z~0.8.Comment: 5 pages, 3 figures, accepted for publication in ApJ
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