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Institution

European Southern Observatory

FacilityGarching bei München, Germany
About: European Southern Observatory is a facility organization based out in Garching bei München, Germany. It is known for research contribution in the topics: Galaxy & Stars. The organization has 3594 authors who have published 16157 publications receiving 823095 citations. The organization is also known as: The European Southern Observatory,ESO & ESO.
Topics: Galaxy, Stars, Star formation, Redshift, Population


Papers
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Journal ArticleDOI
TL;DR: The Survey for Ionization in Neutral Gas Galaxies (SINGG) as mentioned in this paper is a survey of star formation in H I selected galaxies, which consists of H alpha and R-band imaging of a sample of 468 galaxies selected from the H I Parkes All Sky Survey (HIPASS).
Abstract: We introduce the Survey for Ionization in Neutral Gas Galaxies (SINGG), a census of star formation in H I selected galaxies. The survey consists of H alpha and R-band imaging of a sample of 468 galaxies selected from the H I Parkes All Sky Survey (HIPASS). The sample spans three decades in H I mass and is free of many of the biases that affect other star-forming galaxy samples. We present the criteria for sample selection, list the entire sample, discuss our observational techniques, and describe the data reduction and calibration methods. This paper focuses on 93 SINGG targets whose observations have been fully reduced and analyzed to date. The majority of these show a single emission line galaxy (ELG). We see multiple ELGs in 13 fields, with up to four ELGs in a single field. All of the targets in this sample are detected in H alpha, indicating that dormant (non-star-forming) galaxies with M-H I greater than or similar to 3x10(7) M-circle dot are very rare. A database of the measured global properties of the ELGs is presented. The ELG sample spans 4 orders of magnitude in luminosity (H alpha and R band), and H alpha surface brightness, nearly 3 orders of magnitude in R surface brightness and nearly 2 orders of magnitude in H alpha equivalent width (EW). The surface brightness distribution of our sample is broader than that of the Sloan Digital Sky Survey (SDSS) spectroscopic sample, the EW distribution is broader than prism-selected samples, and the morphologies found include all common types of star-forming galaxies (e.g., irregular, spiral, blue compact dwarf, starbursts, merging and colliding systems, and even residual star formation in S0 and Sa spirals). Thus, SINGG presents a superior census of star formation in the local universe suitable for further studies ranging from the analysis of H II regions to determination of the local cosmic star formation rate density.

211 citations

Journal ArticleDOI
Peter A. R. Ade1, M. I. R. Alves2, G. Aniano2, C. Armitage-Caplan3  +223 moreInstitutions (57)
TL;DR: In this paper, the authors use the Planck 353 GHz I, Q, and U Stokes maps as dust templates, and cross-correlate them with the planck and WMAP data at 12 frequencies from 23 to 353 GHz, over circular patches with 10° radius.
Abstract: Planck has mapped the intensity and polarization of the sky at microwave frequencies with unprecedented sensitivity. We use these data to characterize the frequency dependence of dust emission. We make use of the Planck 353 GHz I, Q, and U Stokes maps as dust templates, and cross-correlate them with the Planck and WMAP data at 12 frequencies from 23 to 353 GHz, over circular patches with 10° radius. The cross-correlation analysis is performed for both intensity and polarization data in a consistent manner. The results are corrected for the chance correlation between the templates and the anisotropies of the cosmic microwave background. We use a mask that focuses our analysis on the diffuse interstellar medium at intermediate Galactic latitudes. We determine the spectral indices of dust emission in intensity and polarization between 100 and 353 GHz, for each sky patch. Both indices are found to be remarkably constant over the sky. The mean values, 1.59 ± 0.02 for polarization and 1.51 ± 0.01 for intensity, for a mean dust temperature of 19.6 K, are close, but significantly different (3.6σ). We determine the mean spectral energy distribution (SED) of the microwave emission, correlated with the 353 GHz dust templates, by averaging the results of the correlation over all sky patches. We find that the mean SED increases for decreasing frequencies at ν< 60 GHz for both intensity and polarization. The rise of the polarization SED towards low frequencies may be accounted for by a synchrotron component correlated with dust, with no need for any polarization of the anomalous microwave emission. We use a spectral model to separate the synchrotron and dust polarization and to characterize the spectral dependence of the dust polarization fraction. The polarization fraction (p) of the dust emission decreases by (21 ± 6)% from 353 to 70 GHz. We discuss this result within the context of existing dust models. The decrease in p could indicate differences in polarization efficiency among components of interstellar dust (e.g., carbon versus silicate grains). Our observational results provide inputs to quantify and optimize the separation between Galactic and cosmological polarization.

211 citations

Journal ArticleDOI
TL;DR: In this article, the authors present near-infrared spectroscopy of H? emission lines in a sample of 16 star-forming galaxies at redshifts 2.0 < z < 2.6.
Abstract: We present near-infrared spectroscopy of H? emission lines in a sample of 16 star-forming galaxies at redshifts 2.0 < z < 2.6. Our targets are drawn from a large sample of galaxies photometrically selected and spectroscopically confirmed to lie in this redshift range. We have obtained this large sample with an extension of the broadband UnG color criteria used to identify Lyman break galaxies at z ~ 3. The primary selection criterion for IR spectroscopic observation was proximity to a QSO sight line; we therefore expect the galaxies presented here to be representative of the sample as a whole. Six of the galaxies exhibit spatially extended, tilted H? emission lines; rotation curves for these objects reach mean velocities of ~150 km s-1 at radii of ~6 kpc, without corrections for inclination or any other observational effect. The velocities and radii give a mean dynamical mass of ? 4 ? 1010 M?. We have obtained archival Hubble Space Telescope images for two of these galaxies; they are morphologically irregular. One-dimensional velocity dispersions for the 16 galaxies range from ~50 to ~260 km s-1, and in cases in which we have both virial masses implied by the velocity dispersions and dynamical masses derived from the spatially extended emission lines, they are in rough agreement. We compare our kinematic results with similar measurements made at z ~ 3 and find that both the observed rotational velocities and velocity dispersions tend to be larger at z ~ 2 than at z ~ 3. We also calculate star formation rates (SFRs) from the H? luminosities and compare them with SFRs calculated from the UV continuum luminosity. We find a mean SFRH? of 16 M? yr-1 and an average SFRH?/SFRUV ratio of 2.4, without correcting for extinction. We see moderate evidence for an inverse correlation between the UV continuum luminosity and the ratio SFRH?/SFRUV, such as might be observed if the UV-faint galaxies suffered greater extinction. We discuss the effects of dust and star formation history on the SFRs and conclude that extinction is the most likely explanation for the discrepancy between the two SFRs.

211 citations

Journal ArticleDOI
TL;DR: In this article, scattered light images of the TW Hya disk performed with the Spectro-Polarimetric High-contrast Exoplanet REsearch instrument in Polarimetric Differential Imaging mode at 0.63, 0.79, 1.24, and 1.62 mu m were presented.
Abstract: We present scattered light images of the TW Hya disk performed with the Spectro‐Polarimetric High‐contrast Exoplanet REsearch instrument in Polarimetric Differential Imaging mode at 0.63, 0.79, 1.24, and 1.62 mu m. We also present H2/H3‐band angular differential imaging (ADI) observations. Three distinct radial depressions in the polarized intensity distribution are seen, around approximate to 85, approximate to 21, and less than or similar to 6 au.(21) The overall intensity distribution has a high degree of azimuthal symmetry; the disk is somewhat brighter than average toward the south and darker toward the north‐west. The ADI observations yielded no signifiant detection of point sources in the disk. Our observations have a linear spatial resolution of 1‐2 au, similar to that of recent ALMA dust continuum observations. The submicron‐ sized dust grains that dominate the light scattering in the disk surface are strongly coupled to the gas. We created a radiative transfer disk model with self‐consistent temperature and vertical structure iteration and including grain size‐dependent dust settling. This method may provide independent constraints on the gas distribution at higher spatial resolution than is feasible with ALMA gas line observations. We find that the gas surface density in the ``gaps'' is reduced by approximate to 50% to approximate to 80% relative to an unperturbed model. Should embedded planets be responsible for carving the gaps then their masses are at most a few 10M(circle plus). The observed gaps are wider, with shallower flanks, than expected for planet‐disk interaction with such low‐mass planets. If forming planetary bodies have undergone collapse and are in the ``detached phase,'' then they may be directly observable with future facilities such as the Mid‐Infrared E‐ELT Imager and Spectrograph at the E‐ELT.

211 citations

Journal ArticleDOI
TL;DR: In this paper, the authors present results from a near-infrared narrow-band survey of emission-line galaxies at z = 2.23, using the Wide Field Camera on the United Kingdom Infrared Telescope.
Abstract: We present results from a near-infrared narrow-band survey of emission-line galaxies at z = 2.23, using the Wide Field Camera on the United Kingdom Infrared Telescope. The H2S1 narrow-band filter ( �c = 2.121µm) we employ selects the Hemission line redshifted to z = 2.23, and is thus suitable for selecting 'typical' star forming g alaxies and active galactic nuclei at this epoch. The pilot study was undertaken in the well studied Cosmological Evolution Survey field (COSMOS) and is already the largest near-infrar ed narrow-band survey at this depth, with a line flux limit of FH� � 10 −16 erg s −1 cm −2 over 0.60 square degrees, probing �220× 10 3 Mpc 3 (co-moving) down to a limiting star formation rate of �30M⊙ yr −1 (3�). In this paper we present the results from our pilot survey and evaluate the Hluminosity function and estimate the clustering properties of Hemitters at z = 2.23 from 55 detected galaxies. The integrated luminosity function is used to est imate the volume averaged star formation rate at z = 2.23: �SFR = 0.17 +0.16 −0.09M⊙ yr −1 Mpc −3 for LH� > 10 42 erg s −1 . For the first time, we use the Hstar-formation tracer to reliably constrainSFR out to z = 2.23 demonstrating the rapid increase inSFR out to this redshift as well as confirming the flattening inSFR betweenz � 1-2. In addition to the luminosity distribution, we analyse t he clustering properties of these galaxies. Using the 2-point angular correlation function, !(�), we estimate a real space correlation length of r0 = 4.2 +0.4 −0.2 h −1 Mpc. In comparison to models of clustering which take into account bias evolution, we estimate that these galaxies are hosted by dark matter halos of mass Mhalo � 10 12 M⊙ consistent with the progenitors of the Milky

210 citations


Authors

Showing all 3617 results

NameH-indexPapersCitations
Robert C. Nichol187851162994
Richard S. Ellis169882136011
Rob Ivison1661161102314
Alvio Renzini16290895452
Timothy C. Beers156934102581
Krzysztof M. Gorski132380105912
Emanuele Daddi12958163187
P. R. Christensen12731388445
Mark Dickinson12438966770
Christopher W. Stubbs122622109429
Eva K. Grebel11886383915
Martin Asplund11861252527
Jesper Sollerman11872653436
E. F. van Dishoeck11574249190
Jørgen Christensen-Dalsgaard11458548272
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Performance
Metrics
No. of papers from the Institution in previous years
YearPapers
20233
202231
2021557
2020920
2019759
2018941