Microslit Nod‐Shuffle Spectroscopy: A Technique for Achieving Very High Densities of Spectra

Glazebrook, Karl; Bland-Hawthorn, Joss

doi:10.1086/318625

Cited by 148 publications

(125 citation statements)

References 32 publications

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“…Due to the limited angular extent and high candidate source density of the compact cluster region, we performed the observations in the nod-and-shuffle (N&S) observing mode (Glazebrook & Bland-Hawthorn 2001), using band shuffling (Abraham et al 2004). This observation mode not only allows high-quality sky subtraction but also allows short slits such as the 1 apertures used in this work.…”

Section: Gmos Spectroscopy For Cluster Membership Confirmationmentioning

confidence: 99%

The stellar mass–size relation for cluster galaxies at z = 1 with high angular resolution from the Gemini/GeMS multiconjugate adaptive optics system

Sweet

Sharp

Glazebrook

et al. 2016

Mon. Not. R. Astron. Soc.

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We present the stellar mass -size relation for 49 galaxies within the z = 1.067 cluster SPT-CL J0546−5345, with FWHM ∼80-120 mas K s -band data from the Gemini multiconjugate adaptive optics system (GeMS/GSAOI). This is the first such measurement in a cluster environment, performed at sub-kpc resolution at rest-frame wavelengths dominated by the light of the underlying old stellar populations. The observed stellar mass -size relation is offset from the local relation by 0.21 dex, corresponding to a size evolution proportional to (1 + z) −1.25 , consistent with the literature. The slope of the stellar mass -size relation β = 0.74 ± 0.06, consistent with the local relation. The absence of slope evolution indicates that the amount of size growth is constant with stellar mass. This suggests that galaxies in massive clusters such as SPT-CL J0546−5345 grow via processes that increase the size without significant morphological interference, such as minor mergers and/or adiabatic expansion. The slope of the cluster stellar mass -size relation is significantly shallower if measured in HST /ACS imaging at wavelengths blueward of the Balmer break, similar to rest-frame UV relations at z = 1 in the literature. The stellar mass -size relation must be measured at redder wavelengths, which are more sensitive to the old stellar population that dominates the stellar mass of the galaxies. The slope is unchanged when GeMS K sband imaging is degraded to the resolution of K-band HST/NICMOS resolution but dramatically affected when degraded to K s -band Magellan/FourStar resolution. Such measurements must be made with AO in order to accurately characterise the sizes of compact, z = 1 galaxies.

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Section: Gmos Spectroscopy For Cluster Membership Confirmationmentioning

confidence: 99%

The stellar mass–size relation for cluster galaxies at z = 1 with high angular resolution from the Gemini/GeMS multiconjugate adaptive optics system

Sweet

Sharp

Glazebrook

et al. 2016

Mon. Not. R. Astron. Soc.

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“…A total of six hour-long observations were made. The data were taken using the nod-and-shuffle technique (Glazebrook & Bland-Hawthorn 2001), with the telescope nodded between the on-source position and a blank sky field located 4 away (off the LMC) every 120 s. In total, 3 hr were spent integrating on-source. CuAr spectral calibration images and GCAL flat fields were interspersed with the science observations.…”

Section: Spectroscopic Observationsmentioning

confidence: 99%

Spectral Identification of an Ancient Supernova Using Light Echoes in the Large Magellanic Cloud

Rest¹,

Matheson²,

Blondin³

et al. 2008

ApJ

112

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We report the successful identification of the type of the supernova (SN) responsible for the supernova remnant SNR 0509À675 in the Large Magellanic Cloud ( LMC) using Gemini spectra of surrounding light echoes. The ability to classify outbursts associated with centuries-old remnants provides a new window into several aspects of SN research and is likely to be successful in providing new constraints on additional LMC SNe, as well as their historical counterparts in the Milky Way ( MW ). The combined spectrum of echo light from SNR 0509À675 shows broad emission and absorption lines consistent with a SN spectrum. We create a spectral library consisting of 28 SNe Ia and 6 SNe Ib/c that are time-integrated, dust-scattered by LMC dust, and reddened by the LMC and MW. We fit these SN templates to the observed light echo spectrum using 2 minimization, as well as correlation techniques, and we find that overluminous 1991T-like SNe Ia with Ám 15 < 0:9 match the observed spectrum best. Subject headingg s: ISM: individual (SNR 0509À67.5) -Magellanic Clouds -supernovae: generalsupernova remnants

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“…GMOS has several capabilities that make it ideally suited to studies of galaxy clusters at z ∼ 1. The nod-and-shuffle (n&s) mode (Glazebrook & Bland-Hawthorn 2001) allows excellent sky subtraction at red wavelengths, resulting in much greater efficiency for faint galaxies (as exploited by the GDDS 1 ; Abraham et al 2004). Moreover, the n&s microslits are up to three times smaller than normal slits, allowing them to be placed with a very high surface density.…”

mentioning

confidence: 99%

Gemini Observations of Galaxies in Rich Early Environments (GOGREEN) I: survey description

Balogh

Gilbank

Muzzin

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We describe a new Large Program in progress on the Gemini North and South telescopes: Gemini Observations of Galaxies in Rich Early Environments (GOGREEN). This is an imaging and deep spectroscopic survey of 21 galaxy systems at 1 < z < 1.5, selected to span a factor >10 in halo mass. The scientific objectives include measuring the role of environment in the evolution of low-mass galaxies, and measuring the dynamics and stellar contents of their host haloes. The targets are selected from the SpARCS, SPT, COSMOS, and SXDS surveys, to be the evolutionary counterparts of today's clusters and groups. The new red-sensitive Hamamatsu detectors on GMOS, coupled with the nod-and-shuffle sky subtraction, allow simultaneous wavelength coverage over λ ∼ 0.6-1.05 µm, and this enables a homogeneous and statistically complete redshift survey of galaxies of all types. The spectroscopic sample targets galaxies with AB magnitudes z < 24.25 and [3.6] µm < 22.5, and is therefore statistically complete for stellar masses M * 10 10.3 M , for all galaxy types and over the entire redshift range. Deep, multiwavelength imaging has been acquired over larger fields for most systems, spanning u through K, in addition to deep IRAC imaging at 3.6 µm. The spectroscopy is ∼50 per cent complete as of semester 17A, and we anticipate a final sample of ∼500 new cluster members. Combined with existing spectroscopy on the brighter galaxies from GCLASS, SPT, and other sources, GOGREEN will be a large legacy cluster and field galaxy sample at this redshift that spectroscopically covers a wide range in stellar mass, halo mass, and clustercentric radius.

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Microslit Nod‐Shuffle Spectroscopy: A Technique for Achieving Very High Densities of Spectra

Cited by 148 publications

References 32 publications

The stellar mass–size relation for cluster galaxies at z = 1 with high angular resolution from the Gemini/GeMS multiconjugate adaptive optics system

The stellar mass–size relation for cluster galaxies at z = 1 with high angular resolution from the Gemini/GeMS multiconjugate adaptive optics system

Spectral Identification of an Ancient Supernova Using Light Echoes in the Large Magellanic Cloud

Gemini Observations of Galaxies in Rich Early Environments (GOGREEN) I: survey description

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