The SAURON project - I. The panoramic integral-field spectrograph

Bacon, Roland; Copin, Y.; Monnet, G.; Miller, Bryan W.; Allington‐Smith, J. R.; Bureau, Martin; Carollo, C. M.; Davies, Roger L.; Emsellem, Éric; Küntschner, H.; Peletier, Reynier F.; Verolme, E. K.; Zeeuw, P. T. de

doi:10.1046/j.1365-8711.2001.04612.x

Cited by 604 publications

(488 citation statements)

References 40 publications

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“…The ATLAS 3D project is a volume-limited sample of all nearby early-type galaxies within 42 Mpc selected from the 2MRS with < -M 21.5 K mag (see Cappellari et al 2011). The ATLAS 3D sources have optical IFU spectroscopy using the SAURON instrument (Bacon et al 2001) on the William Herschel Telescope. The near-infrared selection of systematically lower mass systems, combined with their optical ancillary data, makes the ATLAS 3D project the ideal comparison sample for MASSIVE.…”

Section: Atlas 3d : a Representative Lower-mass Comparisonmentioning

confidence: 99%

The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

Goulding

Greene

et al. 2016

ApJ

111

156

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Studies of the physical properties of local elliptical galaxies are shedding new light on galaxy formation. Here we present the hot-gas properties of 33 early-type systems within the MASSIVE galaxy survey that have archival Chandra X-ray observations, and we use these data to derive X-ray luminosities (L X,gas ) and plasma temperatures (T gas ) for the diffuse gas components. We combine this with the ATLAS 3D survey to investigate the X-ray-optical properties of a statistically significant sample of early-type galaxies across a wide range of environments. When X-ray measurements are performed consistently in apertures set by the galaxy stellar content, we deduce that all early types (independent of galaxy mass, environment, and rotational support) follow a universal scaling law such that µL T X,gas gas 4.5 . We further demonstrate that the scatter in L X,gas around both K-band luminosity (L K ) and the galaxy stellar velocity dispersion (s e ) is primarily driven by T gas , with no clear trends with halo mass, radio power, or angular momentum of the stars. It is not trivial to tie the gas origin directly to either stellar mass or galaxy potential. Indeed, our data require a steeper relation between L L , K X,gas , and s e than predicted by standard mass-loss models. Finally, we find that T gas is set by the galaxy potential inside the optical effective radius. We conclude that within the innermost 10-30 kpc region, early types maintain pressure-supported hot gas, with a minimum T gas set by the virial temperature, but the majority show evidence for additional heating.

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Section: Atlas 3d : a Representative Lower-mass Comparisonmentioning

confidence: 99%

The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

Goulding

Greene

et al. 2016

ApJ

111

156

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“…SNIFS provides simultaneous coverage from 3200-9700 Å at a resolution of R;1000. Details of our SNIFS observations and reduction can be found in Bacon et al (2001) and Gaidos et al (2014), which we briefly summarize here. The pipeline detailed in Bacon et al (2001) performs dark, bias, and flat-field corrections, cleans the data of bad pixels and cosmic rays, then fits and extracts the integral field unit spaxels into a one-dimensional spectrum.…”

Section: Uh22 M/supernova Integral Field Spectrograph (Snifs) and Imentioning

confidence: 99%

“…Details of our SNIFS observations and reduction can be found in Bacon et al (2001) and Gaidos et al (2014), which we briefly summarize here. The pipeline detailed in Bacon et al (2001) performs dark, bias, and flat-field corrections, cleans the data of bad pixels and cosmic rays, then fits and extracts the integral field unit spaxels into a one-dimensional spectrum. The Gaidos et al (2014) reduction takes this spectrum and performs flux calibration and telluric correction based on white dwarf standards taken throughout the night and a model of the atmosphere above Maunakea (Buton et al 2013).…”

Section: Uh22 M/supernova Integral Field Spectrograph (Snifs) and Imentioning

confidence: 99%

High-Precision Radio and Infrared Astrometry of LSPM J1314+1320ab. Ii. Testing Pre-Main-Sequence Models at the Lithium Depletion Boundary With Dynamical Masses

Dupuy

Forbrich

Rizzuto

et al. 2016

ApJ

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We present novel tests of pre-main-sequence models based on individual dynamical masses for the M7 binary LSPMJ1314+1320AB. Joint analysis of Keck adaptive optics astrometric monitoring along with Very Long Baseline Array radio data from a companion paper yield component masses of 92.8±0.6 M Jup (0.0885±0.0006 M ☉ ) and 91.7±1.0 M Jup (0.0875±0.0010 M ☉ ) and a parallactic distance of 17.249±0.013 pc. We find component luminosities consistent with the system being coeval at 80.8±2.5 Myr, according to BHAC15 evolutionary models. The presence of lithium is consistent with model predictions, marking the first test of the theoretical lithium depletion boundary using ultracool dwarfs of known mass. However, we find that the evolutionary model-derived average effective temperature (2950±5 K) is 180 K hotter than that given by a spectral type-T eff relation based on BT-Settl models (2770±100 K). We suggest that the dominant source of this discrepancy is model radii being too small by ≈13%. In a test mimicking the typical application of models by observers, we derive masses on the H-R diagram using luminosity and BT-Settl temperature. The estimated masses are lower by -(2.0σ) than we measure dynamically and would imply that this is a system of ≈50 M Jup brown dwarfs, highlighting the large systematic errors possible in H-R diagram properties. This is the first time masses have been measured for ultracool ( M6) dwarfs displaying spectral signatures of low gravity. Based on features in the infrared, LSPMJ1314+1320AB appears to have higher gravity than typical Pleiades and ABDor members, opposite the expectation given its younger age. The components of LSPMJ1314+1320AB are now the nearest, lowest mass pre-main-sequence stars with direct mass measurements.

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“…It consists of a high-throughput wide-band pure-lenslet integral field spectrograph (IFS, "à la TIGER"; Bacon et al 1995Bacon et al , 2001), a multifilter photometric channel to image the field surrounding the IFS for atmospheric transmission monitoring simultaneous with spectroscopy, and an acquisition/guiding channel. The IFS possesses a fully filled 6.…”

Section: The Supernova Integral Field Spectrograph and Data Reductionmentioning

confidence: 99%

Atmospheric extinction properties above Mauna Kea from the Nearby SuperNova Factory spectro-photometric data set

Buton

Copin

Aldering

et al. 2012

A&A

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We present a new atmospheric extinction curve for Mauna Kea spanning 3200-9700 Å. It is the most comprehensive to date, being based on some 4285 standard star spectra obtained on 478 nights spread over a period of 7 years obtained by the Nearby SuperNova Factory using the SuperNova Integral Field Spectrograph. This mean curve and its dispersion can be used as an aid in calibrating spectroscopic or imaging data from Mauna Kea, and in estimating the calibration uncertainty associated with the use of a mean extinction curve. Our method for decomposing the extinction curve into physical components, and the ability to determine the chromatic portion of the extinction even on cloudy nights, is described and verified over the wide range of conditions sampled by our large dataset. We demonstrate good agreement with atmospheric science data obtain at nearby Mauna Loa Observatory, and with previously published measurements of the extinction above Mauna Kea.

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The SAURON project - I. The panoramic integral-field spectrograph

Cited by 604 publications

References 40 publications

The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

High-Precision Radio and Infrared Astrometry of LSPM J1314+1320ab. Ii. Testing Pre-Main-Sequence Models at the Lithium Depletion Boundary With Dynamical Masses

Atmospheric extinction properties above Mauna Kea from the Nearby SuperNova Factory spectro-photometric data set

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