79 research outputs found
Measuring star formation in high-z massive galaxies: A mid-infrared to submillimeter study of the GOODS NICMOS Survey sample
We present measurements of the mean mid-infrared-to-submillimeter flux
densities of massive (M\ast \approx 2 \times 10^11 Msun) galaxies at redshifts
1.7 < z < 2.9, obtained by stacking positions of known objects taken from the
GOODS NICMOS Survey (GNS) catalog on maps: at 24 {\mu}m (Spitzer/MIPS); 70,
100, and 160{\mu}m (Herschel/PACS); 250, 350, 500{\mu}m (BLAST); and 870{\mu}m
(LABOCA). A modified blackbody spectrum fit to the stacked flux densities
indicates a median [interquartile] star-formation rate of SFR = 63 [48, 81]
Msun yr^-1 . We note that not properly accounting for correlations between
bands when fitting stacked data can significantly bias the result. The galaxies
are divided into two groups, disk-like and spheroid-like, according to their
Sersic indices, n. We find evidence that most of the star formation is
occurring in n \leq 2 (disk-like) galaxies, with median [interquartile] SFR =
122 [100,150] Msun yr^-1, while there are indications that the n > 2
(spheroid-like) population may be forming stars at a median [interquartile] SFR
= 14 [9,20] Msun yr^-1, if at all. Finally, we show that star formation is a
plausible mechanism for size evolution in this population as a whole, but find
only marginal evidence that it is what drives the expansion of the
spheroid-like galaxies.Comment: Accepted by MNRAS. 10 pages, 3 figures, 3 table
Cold Dust but Warm Gas in the Unusual Elliptical Galaxy NGC 4125
Data from the Herschel Space Observatory have revealed an unusual elliptical galaxy, NGC 4125, which has strong and extended submillimeter emission from cold dust but only very strict upper limits to its CO and Hi emission. Depending on the dust emissivity, the total dust mass is 2-5 x 10(6) M-circle dot. While the neutral gas-to-dust mass ratio is extremely low (= 10(4) K faster than the dust is evaporated. If galaxies like NGC 4125, where the far-infrared emission does not trace neutral gas in the usual manner, are common at higher redshift, this could have significant implications for our understanding of high redshift galaxies and galaxy evolution.Canadian Space AgencyNatural Sciences and Engineering Research Council of CanadaAgenzia Spaziale Italiana (ASI) I/005/11/0BMVIT (Austria)ESA-PRODEX (Belgium)CEA/CNES (France)DLR (Germany)ASI/INAF (Italy)CICYT/MCYT (Spain)CSA (Canada)NAOC (China)CEA, (France)CNES (France)CNRS (France)ASI (Italy)MCINN (Spain)SNSB (Sweden)STFC (UK)NASA (USA)National Aeronautics and Space AdministrationAstronom
The Herschel Exploitation of Local Galaxy Andromeda (HELGA) II: Dust and Gas in Andromeda
We present an analysis of the dust and gas in Andromeda, using Herschel
images sampling the entire far-infrared peak. We fit a modified-blackbody model
to ~4000 quasi-independent pixels with spatial resolution of ~140pc and find
that a variable dust-emissivity index (beta) is required to fit the data. We
find no significant long-wavelength excess above this model suggesting there is
no cold dust component. We show that the gas-to-dust ratio varies radially,
increasing from ~20 in the center to ~70 in the star-forming ring at 10kpc,
consistent with the metallicity gradient. In the 10kpc ring the average beta is
~1.9, in good agreement with values determined for the Milky Way (MW). However,
in contrast to the MW, we find significant radial variations in beta, which
increases from 1.9 at 10kpc to ~2.5 at a radius of 3.1kpc and then decreases to
1.7 in the center. The dust temperature is fairly constant in the 10kpc ring
(ranging from 17-20K), but increases strongly in the bulge to ~30K. Within
3.1kpc we find the dust temperature is highly correlated with the 3.6 micron
flux, suggesting the general stellar population in the bulge is the dominant
source of dust heating there. At larger radii, there is a weak correlation
between the star formation rate and dust temperature. We find no evidence for
'dark gas' in M31 in contrast to recent results for the MW. Finally, we
obtained an estimate of the CO X-factor by minimising the dispersion in the
gas-to-dust ratio, obtaining a value of (1.9+/-0.4)x10^20 cm^-2 [K kms^-1]^-1.Comment: 19 pages, 18 figures. Submitted to ApJ April 2012; Accepted July 201
Timescale of Mass Accretion in Pre-Main-Sequence Stars
We present initial result of a large spectroscopic survey aimed at measuring
the timescale of mass accretion in young, pre-main-sequence stars in the
spectral type range K0 - M5. Using multi-object spectroscopy with VIMOS at the
VLT we identified the fraction of accreting stars in a number of young stellar
clusters and associations of ages between 1 - 50 Myr. The fraction of accreting
stars decreases from ~60% at 1.5 - 2 Myr to ~2% at 10 Myr. No accreting stars
are found after 10 Myr at a sensitivity limit of Msun yr-1. We
compared the fraction of stars showing ongoing accretion (f_acc) to the
fraction of stars with near-to-mid infrared excess (f_IRAC). In most cases we
find f_acc < f_IRAC, i.e., mass accretion appears to cease (or drop below
detectable level) earlier than the dust is dissipated in the inner disk. At 5
Myr, 95% of the stellar population has stopped accreting material at a rate of
> 10^{-11} Msun yr-1, while ~20% of the stars show near-infrared excess
emission. Assuming an exponential decay, we measure a mass accretion timescale
(t_acc) of 2.3 Myr, compared to a near-to-mid infrared excess timescale
(t_IRAC) of 2.9 Myr. Planet formation, and/or migration, in the inner disk
might be a viable mechanism to halt further accretion onto the central star on
such a short timescale.Comment: Accepted for publicatio
Dust heating sources in galaxies: the case of M33 (HERM33ES)
Dust emission is one of the main windows to the physics of galaxies and to
star formation as the radiation from young, hot stars is absorbed by the dust
and reemitted at longer wavelengths. The recently launched Herschel satellite
now provides a view of dust emission in the far-infrared at an unequaled
resolution and quality up to 500 \mu m. In the context of the Herschel HERM33ES
open time key project, we are studying the moderately inclined Scd local group
galaxy M33 which is located only 840 kpc away. In this article, using Spitzer
and Herschel data ranging from 3.6 \mu m to 500 \mu m, along with HI, H\alpha\
maps, and GALEX ultraviolet data we have studied the emission of the dust at
the high spatial resolution of 150 pc. Combining Spitzer and Herschel bands, we
have provided new, inclination corrected, resolved estimators of the total
infrared brightness and of the star formation rate from any combination of
these bands. The study of the colors of the warm and cold dust populations
shows that the temperature of the former is, at high brightness, dictated by
young massive stars but, at lower brightness, heating is taken over by the
evolved populations. Conversely, the temperature of the cold dust is tightly
driven by the evolved stellar populations.Comment: 29 pages, 12 figures, accepted for publication in A
A Compact Cluster of Massive Red Galaxies at a Redshift of 1.51
We describe a compact cluster of massive red galaxies at z=1.51 discovered in
one of the Gemini Deep Deep Survey (GDDS) fields. Deep imaging with the Near
Infrared Camera and Multi Object Spectrometer (NICMOS) on the Hubble Space
Telescope reveals a high density of galaxies with red optical to near-IR colors
surrounding a galaxy with a spectroscopic redshift of 1.51. Mid-IR imaging with
Infrared Array Camera (IRAC) on the Spitzer Space telescope shows that these
galaxies have spectral energy distributions that peak between 3.6 and 4.5
microns. Fits to 12-band photometry reveal 12 or more galaxies with spectral
shapes consistent with z = 1.51. Most are within ~170 co-moving kpc of the GDDS
galaxy. Deep F814W images with the Advanced Camera for Surveys (ACS) on HST
reveal that these galaxies are a mix of early-type galaxies, disk galaxies and
close pairs. The total stellar mass enclosed within a sphere of 170 kpc in
radius is > 8E+11 solar masses. The colors of the most massive galaxies are
close to those expected from passive evolution of simple stellar populations
(SSP) formed at much higher redshifts. We suggest that several of these
galaxies will merge to form a single, very massive galaxy by the present day.
This system may represent an example of a short-lived dense group or cluster
core typical of the progenitors of massive clusters in the present day and
suggests the red sequence was in place in over-dense regions at early times.Comment: 14 pages, 6 figures, submitted to ApJ Letter
The Gemini Deep Deep Survey: VIII. When Did Early-type Galaxies Form?
We have used the Hubble Space Telescope's Advanced Camera for Surveys (Ford et al. 2003) to measure the cumulative mass density in morphologically-selected early-type galaxies over the redshift range 0.8 < z < 1.7. Our imaging data set covers four well-separated sight-lines, and is roughly intermediate (in terms of both depth and area) between the GOODS/GEMS imaging data, and the images obtained in the Hubble Deep Field campaigns. Our images contain 144 galaxies with ultra-deep spectroscopy obtained as part of the Gemini Deep Deep Survey. These images have been analyzed using a new purpose-written morphological analysis code which improves the reliability of morphological classifications by adopting a 'quasi-Petrosian' image thresholding technique. We find that at z \~ 1 about 80% of the stars living in the most massive galaxies reside in early-type systems. This fraction is similar to that seen in the local Universe. However, we detect very rapid evolution in this fraction over the range 0.8 < z < 1.7, suggesting that over this redshift range the strong morphology-mass relationship seen in the nearby Universe is beginning to fall into place. By comparing our images to published spectroscopic classifications, we show that little ambiguity exists in connecting spectral classes to morphological classes for spectroscopically quiescent systems. However, the mass density function of early-type galaxies is evolving more rapidly than that of spectroscopically quiescent systems, which we take as further evidence that we are witnessing the formation of massive early-type galaxies over the 0.8 < z < 1.7 redshift range
The Herschel Stripe 82 Survey (HerS): maps and early catalog
We present the first set of maps and band-merged catalog from the Herschel Stripe 82 Survey (HerS). Observations at 250, 350, and 500μm were taken with the Spectral and Photometric Imaging Receiver instrument aboard the Herschel Space Observatory. HerS covers 79deg 2 along the SDSS Stripe 82 to an average depth of 13.0, 12.9, and 14.8mJybeam −1 (including confusion) at 250, 350, and 500μm, respectively. HerS was designed to measure correlations with external tracers of the dark matter density field—either point-like (i.e., galaxies selected from radio to X-ray) or extended (i.e., clusters and gravitational lensing)—in order to measure the bias and redshift distribution of intensities of infrared-emitting dusty star-forming galaxies and active galactic nuclei. By locating HerS in Stripe 82, we maximize the overlap with available and upcoming cosmological surveys. The band-merged catalog contains 3.3 × 10 4 sources detected at a significance of ?3σ (including confusion noise). The maps and catalog are available at http://www.astro.caltech.edu/hers/
The Herschel Reference Survey: Dust in Early-Type Galaxies and Across the Hubble Sequence
We present Herschel observations of 62 Early-Type Galaxies (ETGs), including
39 galaxies morphologically classified as S0+S0a and 23 galaxies classified as
ellipticals using SPIRE at 250, 350 and 500 microns (and PACS 100 and 160
microns for 19 sources) as part of the volume-limited Herschel Reference
Survey. We detect dust emission in 24% of the ellipticals and 62% of the S0s.
The mean temperature of the dust is 23.9+/-0.8 K, warmer than that found for
late-type galaxies in the Virgo Cluster. Including the non-detections, the mean
dust mass is log(Mdust) = 5.9+/-0.1 and 5.2+/-0.1 Msun for the S0s and
elliptical galaxies respectively. The mean dust-to-stellar mass is
log(Mdust/Mstar) = -4.4+/-0.1 (S0s) and -5.8+/-0.1 (ellipticals). Virtually all
the galaxies lie close to the red sequence yet the large number of detections
of cool dust, the gas-to-dust ratios and the ratios of far-infrared to radio
emission all suggest that many ETGs contain a cool interstellar medium similar
to that in late-type galaxies. The mean dust-to-stellar mass ratio for S0s is
approximatly a factor of ten less than for early-type spirals and the sizes of
the dust sources in the S0s are also much smaller. We show that the difference
cannot be explained by either the different bulge-to-disk ratios or
environmental effects such as ram-pressure stripping. The wide range in the
dust-to-stellar mass ratio for ETGs and the lack of a correlation between dust
mass and optical luminosity suggest that much of the dust in the ETGs detected
by Herschel has been acquired as the result of gravitational interactions;
these interactions are unlikely to have had a major effect on the stellar
masses of the ETGs. The Herschel observations tentatively suggest that in the
most massive ETGs, the mass of the interstellar medium is unconnected to the
evolution of the stellar populations.Comment: 28 Pages, 12 Figures. Submitted to ApJ December 2011; accepted
January 201
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