IMACS: The Inamori-Magellan Areal Camera and Spectrograph on Magellan-Baade

Dressler, Alan; Bigelow, Bruce C.; Hare, Tyson; Sutin, Brian M.; Thompson, I. B.; Burley, Greg; Epps, Harland W.; Oemler, A.; Bagish, Alan; Birk, Christoph; Clardy, K. D.; Gunnels, Steve; Kelson, Daniel D.; Shectman, Stephen; Osip, D. J.

doi:10.1086/658908

Cited by 258 publications

(210 citation statements)

References 16 publications

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“…We are performing an integral field spectroscopy survey of these 29 AGNs using three different instruments: the GMOS IFU (Allington-Smith et al 2002) on Gemini-North (six sources, presented here), the Inamori MAgellan Cassegrain Spectrograph (IMACS) IFU (Dressler et al 2011) on the 6 m Magellan-Baade telescope (nine sources), and the SuperNova Integral Field Spectrograph (SNIFS) IFU (Aldering et al 2002;Lantz et al 2004) on the 2.2 m University of Hawaii telescope (14 sources). Given the significant differences in spatial and spectral resolution and the achieved signal-to-noise ratio (S/N) among the three data sets, we present first the results using the highest-quality Gemini GMOS-N data.…”

Section: Sample Selectionmentioning

confidence: 99%

Unraveling the Complex Structure of Agn-Driven Outflows. I. Kinematics and Sizes

Karouzos

Woo

Bae

2016

ApJ

105

156

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Outflows driven by active galactic nuclei (AGNs) are often invoked as agents of the long-sought AGN feedback. Yet, characterizing and quantifying the impact on their host galaxies has been challenging. We present Gemini Multi-Object Spectrograph integral field unit data of six local (z 0.1 < ) and luminous (L 10In the first of a series of papers, we investigate the kinematics and constrain the size of the outflows. The ionized gas kinematics can be described as a superposition of a gravitational component that follows the stellar motion and an outflow-driven component that shows large velocity (up to 600 km s −1 ) and large velocity dispersion (up to 800 km s −1 ). Using the spatially resolved measurements of the gas, we kinematically measure the size of the outflow, which is found to be between 1.3 and 2.1 kpc. Owingto the lack of a detailed kinematic analysis, previous outflow studies likely overestimate their size by up to more than a factor of two, depending on how the size is estimated and whether the [O III] or Hα emission line is used. The relatively small size of the outflows for all six of our objects casts doubts on their potency as a mechanism for negative AGN feedback.

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Section: Sample Selectionmentioning

confidence: 99%

Unraveling the Complex Structure of Agn-Driven Outflows. I. Kinematics and Sizes

Karouzos

Woo

Bae

2016

ApJ

105

156

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“…The handling of the data is similar to that in the XMM-LSS field (Kelson et al 2014), though our deep DECam photometry provides for more uniform completeness as a function of magnitude. Briefly, CSI targets were selected in the Spitzer IRAC 3.6 µm band with magnitudes brighter than 21 AB mag and observed with the Uniform Dispersion Prism (UDP) on IMACS (Dressler et al 2011) at Magellan. Redshifts were measured by fitting the available spectrophotometry (spectrum + ugrizJHK) with SEDs generated from stellar population synthesis models.…”

Section: Csi Spectroscopy and Completenessmentioning

confidence: 99%

THE STELLAR MASS–HALO MASS RELATION FOR LOW-MASS X-RAY GROUPS AT 0.5< z < 1 IN THE CDFS WITH CSI

Patel¹,

Kelson²,

Williams³

et al. 2015

ApJ

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Since z ∼ 1, the stellar mass density locked in low mass groups and clusters has grown by a factor of ∼ 8. Here we make the first statistical measurements of the stellar mass content of low mass X-ray groups at 0.5 < z < 1, enabling the calibration of stellar-to-halo mass scales for wide-field optical and infrared surveys. Groups are selected from combined Chandra and XM M − N ewton X-ray observations in the Chandra Deep Field South (CDFS). These ultra-deep observations allow us to identify bona fide low mass groups at high redshift and enable measurements of their total halo masses. We compute aggregate stellar masses for these halos using galaxies from the CarnegieSpitzer-IMACS (CSI) spectroscopic redshift survey. Stars comprise ∼ 3 − 4% of the total mass of group halos with masses 10 12.8 < M 200 /M ⊙ < 10 13.5 (about the mass of Fornax and 1/50th the mass of Virgo). Complementing our sample with higher mass halos at these redshifts, we find that the stellar-to-halo mass ratio decreases toward higher halo masses, consistent with other work in the local and high redshift universe. The observed scatter about the stellar-halo mass relation is σ ∼ 0.25 dex, which is relatively small and suggests that total group stellar mass can serve as a rough proxy for halo mass. We find no evidence for any significant evolution in the stellar-halo mass relation since z 1. Quantifying the stellar content in groups since this epoch is critical given that hierarchical assembly leads to such halos growing in number density and hosting increasing shares of quiescent galaxies.

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“…We observed the ChaMPlane field containing CBS 7 in multi-object slit spectroscopy mode with the Inamori-Magellan Areal Camera & Spectrograph (IMACS; Dressler et al 2011) at the Baade Magellan Telescope on 2010 August 30 with the f/4 camera and a 300 lines mm −1 grating (3650-9740 Å, 0.743 Å pixel −1 ). We obtained three observations of 30 minutes (hereafter sp1, sp2, and sp3) for 46 targets.…”

Section: Multi-object Optical Spectroscopymentioning

confidence: 99%

SPECTROSCOPIC FOLLOW-UP OF X-RAY SOURCES IN THE ChaMPlane SURVEY: IDENTIFICATION OF A NEW CATACLYSMIC VARIABLE

Servillat

Grindlay

Berg

et al. 2012

ApJ

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We present a multi-object optical spectroscopy follow-up study of X-ray sources in a field along the Galactic plane (l = 327.• 42, b = 2.• 26) which is part of the Chandra Multi-wavelength Plane survey (ChaMPlane). We obtained spectra for 46 stars, including 15 likely counterparts to X-ray sources, and sources showing an Hα color excess. This has led to the identification of a new cataclysmic variable (CV), CXOPS J154305.5-522709, also named ChaMPlane Bright Source 7 (CBS 7), and we identified eight X-ray sources in the field as active late-type stars. CBS 7 was previously studied in X-rays and showed a hard spectrum and two periods: 1.22 ± 0.08 hr and 2.43 ± 0.26 hr. We present here clear evidence that the source is a CV through the detection of H, He i, and He ii emission lines in its optical spectrum. The hard X-ray spectrum and the presence of the He ii λ4686 in emission with a large equivalent width suggest a magnetic CV. The near-infrared counterpart is significantly variable, and we found a period consistent with the longest X-ray period at 2.39 ± 0.05 hr but not the shortest X-ray period. If this period is the orbital period, this would place the system in the CV period gap. The possible orbital period suggests a dM4 ± 1 companion star. The distance is then estimated to be ∼1 kpc. The system could be a relatively hard and X-ray luminous polar or an intermediate polar, possibly nearly synchronous.

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IMACS: The Inamori-Magellan Areal Camera and Spectrograph on Magellan-Baade

Cited by 258 publications

References 16 publications

Unraveling the Complex Structure of Agn-Driven Outflows. I. Kinematics and Sizes

Unraveling the Complex Structure of Agn-Driven Outflows. I. Kinematics and Sizes

THE STELLAR MASS–HALO MASS RELATION FOR LOW-MASS X-RAY GROUPS AT 0.5< z < 1 IN THE CDFS WITH CSI

SPECTROSCOPIC FOLLOW-UP OF X-RAY SOURCES IN THE ChaMPlane SURVEY: IDENTIFICATION OF A NEW CATACLYSMIC VARIABLE

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