The Diskmass Survey. I. Overview

Bershady, Matthew A.; Verheijen, Marc; Swaters, R. A.; Andersen, David R.; Westfall, Kyle B.; Martinsson, Thomas P. K.

doi:10.1088/0004-637x/716/1/198

Cited by 222 publications

(227 citation statements)

References 76 publications

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“…Closer galaxies with larger angular sizes will have values of R 25 that are outside the FoV, while the S/N of small (and faint) galaxies will be not enough for most 2D studies. Our study therefore illustrate the importance of the sample selection not only in terms of volume and limiting magnitude, but also the apparent size of galaxies as previous works have shown (e.g., Bershady et al 2010a).…”

Section: Spatially Resolved Propertiessupporting

confidence: 84%

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Integral field spectroscopy of a sample of nearby galaxies

Mármol-Queraltó

Sanchez

Marino

et al. 2011

A&A

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Aims. Integral field spectroscopy (IFS) is a powerful approach to studying nearby galaxies since it enables a detailed analysis of their resolved physical properties. Here we present our study of a sample of nearby galaxies selected to exploit the two-dimensional information provided by the IFS. Methods. We observed a sample of 48 galaxies from the local universe with the PPaK integral field spectroscopy unit (IFU), of the PMAS spectrograph, mounted at the 3.5 m telescope at Calar Alto Observatory (Almeria, Spain). Two different setups were used during these studies (low -V300 -and medium -V600 -resolution mode) covering a spectral range of around 3700-7000 ÅÅ. We developed a full automatic pipeline for the data reduction, which includes an analysis of the quality of the final data products. We applied a decoupling method to obtain the ionised gas and stellar content of these galaxies, and derive the main physical properties of the galaxies. To assess the accuracy in the measurements of the different parameters, we performed a set of simulations to derive the expected relative errors obtained with these data. In addition, we extracted spectra for two types of aperture, one central and another integrated over the entire galaxy, from the datacubes. The main properties of the stellar populations and ionised gas of these galaxies and an estimate of their relative errors are derived from those spectra, as well as from the whole datacubes. Results. We compare the central spectrum extracted from our datacubes and the SDSS spectrum for each of the galaxies for which this is possible, and find close agreement between the derived values for both samples. We find differences on the properties of galaxies when comparing a central and an integrated spectra, showing the effects of the extracted aperture on the interpretation of the data. Finally, we present two-dimensional maps of some of the main properties derived with the decoupling procedure.

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Section: Spatially Resolved Propertiessupporting

confidence: 84%

“…Two different sample selections are explored in this work: (1) galaxies extracted from the SDSS DR4 imaging sample brighter than r < 15.75 mag and of redshift 0.005 < z < 0.025 (selection in volume and limiting magnitude) and (2) face-on disk galaxies included in the DiskMass Survey (DMS, Bershady et al 2010a;Verheijen, priv. comm.…”

Section: Samplementioning

confidence: 99%

Integral field spectroscopy of a sample of nearby galaxies

Mármol-Queraltó

Sanchez

Marino

et al. 2011

A&A

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“…Colina et al (1999) and de Zeeuw et al (2002), such integral-field spectroscopy has provided a wealth of information. In the nearby universe, for instance, observations from the DiskMass survey (Bershady et al 2010) have indicated that late-type galaxies tend to have sub-maximal disks (Bershady et al 2011), while Atlas-3D observations (Cappellari et al 2011a) showed that early-type galaxies frequently have rapidly rotating components (especially in low-density environments; Cappellari et al 2011b). In the more distant universe, integral-field spectroscopic observations have been crucial in establishing the prevalence of high gas-phase velocity dispersions (e.g., Förster Schreiber et al 2009;Law et al 2009Law et al , 2012Wisnioski et al 2015), giant kiloparsec-sized clumps of young stars (e.g., Förster Schreiber et al 2011), and powerful nuclear outflows (Förster Schreiber et al 2014) that may indicate fundamental differences in gas accretion mechanisms in the young universe (e.g., Dekel et al 2009).…”

Section: Introductionmentioning

confidence: 99%

THE DATA REDUCTION PIPELINE FOR THE SDSS-IV MaNGA IFU GALAXY SURVEY

Law¹,

Cherinka²,

Yan³

et al. 2016

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Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) is an optical fiber-bundle integral-field unit (IFU) spectroscopic survey that is one of three core programs in the fourth-generation Sloan Digital Sky Survey (SDSS-IV). With a spectral coverage of 3622-10354 Å and an average footprint of ∼500 arcsec 2 per IFU the scientific data products derived from MaNGA will permit exploration of the internal structure of a statistically large sample of 10,000 low-redshift galaxies in unprecedented detail. Comprising 174 individually pluggable science and calibration IFUs with a near-constant data stream, MaNGA is expected to obtain ∼100 million raw-frame spectra and ∼10 million reduced galaxy spectra over the six-year lifetime of the survey. In this contribution, we describe the MaNGA Data Reduction Pipeline algorithms and centralized metadata framework that produce skysubtracted spectrophotometrically calibrated spectra and rectified three-dimensional data cubes that combine individual dithered observations. For the 1390 galaxy data cubes released in Summer 2016 as part of SDSS-IV Data Release 13, we demonstrate that the MaNGA data have nearly Poisson-limited sky subtraction shortward of ∼8500 Å and reach a typical 10σ limiting continuum surface brightness μ=23.5 AB arcsec −2 in a five-arcseconddiameter aperture in the g-band. The wavelength calibration of the MaNGA data is accurate to 5 km s −1 rms, with a median spatial resolution of 2.54 arcsec FWHM (1.8 kpc at the median redshift of 0.037) and a median spectral resolution of σ=72 km s −1 .

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“…One of the main goals of the DiskMass Survey (DMS; Bershady et al 2010a, hereafter Paper I) is to break the diskhalo degeneracy using stellar and gas kinematics to determine the dynamical mass-to-light ratio of the galaxy disk (Υ dyn ). For a locally isothermal disk…”

Section: Introductionmentioning

confidence: 99%

The DiskMass Survey

Martinsson

Verheijen

Westfall

et al. 2013

A&A

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197

225

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We present dynamically-determined rotation-curve mass decompositions of 30 spiral galaxies, which were carried out to test the maximum-disk hypothesis and to quantify properties of their dark-matter halos. We used measured vertical velocity dispersions of the disk stars to calculate dynamical mass surface densities (Σ dyn ). By subtracting our observed atomic and inferred molecular gas mass surface densities from Σ dyn , we derived the stellar mass surface densities (Σ * ), and thus have absolute measurements of all dominant baryonic components of the galaxies. Using K-band surface brightness profiles (I K ), we calculated the K-band mass-to-light ratio of the stellar disks (Υ * = Σ * /I K ) and adopted the radial mean (Υ * ) for each galaxy to extrapolate Σ * beyond the outermost kinematic measurement. The derived Υ * of individual galaxies are consistent with all galaxies in the sample having equal Υ * . We find a sample average and scatter of Υ * = 0.31 ± 0.07. Rotation curves of the baryonic components were calculated from their deprojected mass surface densities. These were used with circular-speed measurements to derive the structural parameters of the dark-matter halos, modeled as either a pseudo-isothermal sphere (pISO) or a Navarro-Frenk-White (NFW) halo. In addition to our dynamically determined mass decompositions, we also performed alternative rotation-curve decompositions by adopting the traditional maximumdisk hypothesis. However, the galaxies in our sample are submaximal, such that at 2.2 disk scale lengths (h R ) the ratios between the baryonic and total rotation curves (F 2.2h R b ) are less than 0.75. We find this ratio to be nearly constant between 1-6h R within individual galaxies. We find a sample average and scatter of F 2.2h R b = 0.57 ± 0.07, with trends of larger F 2.2h R b for more luminous and higher-surface-brightness galaxies. To enforce these being maximal, we need to scale Υ * by a factor 3.6 on average. In general, the dark-matter rotation curves are marginally better fit by a pISO than by an NFW halo. For the nominal-Υ * (submaximal) case, we find that the derived NFW-halo parameters have values consistent with ΛCDM N-body simulations, suggesting that the baryonic matter in our sample of galaxies has only had a minor effect on the dark-matter distribution. In contrast, maximum-Υ * decompositions yield halo-concentration parameters that are too low compared to the ΛCDM simulations.

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The Diskmass Survey. I. Overview

Cited by 222 publications

References 76 publications

Integral field spectroscopy of a sample of nearby galaxies

Integral field spectroscopy of a sample of nearby galaxies

THE DATA REDUCTION PIPELINE FOR THE SDSS-IV MaNGA IFU GALAXY SURVEY

The DiskMass Survey

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