The multi-object double spectrographs for the Large Binocular Telescope

Pogge, Richard W.; Atwood, Bruce; Brewer, D. F.; Byard, P. L.; Derwent, Mark; Gonzàlez, R.; Martini, Paul; Mason, Jerry; O’Brien, T. P.; Osmer, Patrick S.; Pappalardo, Daniel; Steinbrecher, D.; Teiga, E. J.; Zhelem, Ross

doi:10.1117/12.857215

Cited by 129 publications

(31 citation statements)

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“…On 2016 March 9 and 10 we observed in mostly clear conditions using the Multi-object Double Spectrograph (MODS; Pogge et al 2010) on the Large Binocular Telescope (LBT) prior to the binocular mode being operational. Because UDGs have relatively flat surface brightness profiles, we opted to use a wide slit to increase the amount of light collected, at the expense of spectral resolution.…”

Section: Datamentioning

confidence: 99%

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Spectroscopy of Ultra-diffuse Galaxies in the Coma Cluster

Kadowaki

Zaritsky

Donnerstein

2017

ApJL

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We present spectra of five ultra-diffuse galaxies (UDGs) in the vicinity of the Coma cluster obtained with the Multi-object Double Spectrograph on the Large Binocular Telescope. We confirm four of these as members of the cluster, quintupling the number of spectroscopically confirmed systems. Like the previously confirmed large (projected half-light radius >4.6 kpc) UDG, DF44, the systems we targeted all have projected half-light radii 2.9 kpc > . As such, we spectroscopically confirm a population of physically large UDGs in the Coma cluster. The remaining UDG is located in the field, about 45 Mpc behind the cluster. We observe Balmer and Ca II H and K absorption lines in all of our UDG spectra. By comparing the stacked UDG spectrum against stellar population synthesis models, we conclude that, on average, these UDGs are composed of metal-poor stars ([Fe/H]−1.5). We also discover the first UDG with [O II] and [O III] emission lines within a clustered environment, demonstrating that not all cluster UDGs are devoid of gas and sources of ionizing radiation.

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Section: Datamentioning

confidence: 99%

“…We reduced the spectra using the MODS data reduction pipeline (Pogge et al 2010). Reduction includes the standard steps of overscan correction, 2D bias subtraction, dark current subtraction, flat fielding, wavelength calibration, sky subtraction, flux calibration, and extraction.…”

Section: Datamentioning

confidence: 99%

Spectroscopy of Ultra-diffuse Galaxies in the Coma Cluster

Kadowaki

Zaritsky

Donnerstein

2017

ApJL

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“…This spectroscopic campaign was carried out using several instruments at different telescopes: EFOSC2 at the NTT telescope in La Silla, the Focal Reducer / Low-Dispersion Spectrograph 2 (FORS2; Appenzeller & Rupprecht 1992) at the Very Large Telescope (VLT), the Folded-Port Infrared Echellette (FIRE; Simcoe et al 2008Simcoe et al , 2013 spectrometer and the Low-Dispersion Survey Spectrograph (LDSS3) at the Baade and Clay Telescopes at Las Campanas Observatory, the Low-Resolution Imaging Spectrometer (LRIS; Oke et al 1995) at the Keck I 10 m Telescope on Mauna Kea, the Double Spectrograph (DBSP; Oke & Gunn 1982) on the 200 inch (5 m) Hale Telescope at Palomar Observatory (P200), the Red-Channel Spectrograph (Schmidt et al 1989) on the 6.5 m MMT Telescope, the Cassegrain TWIN Spectrograph at the 3.5 m Calar Alto Telescope (CAHA 3.5 m), and the Multi-object Double Spectrograph (MODS; Pogge et al 2010) and LUCI spectrograph (Seifert et al 2003) at the Large Binocular Telescope (LBT).…”

Section: Spectroscopymentioning

confidence: 99%

THE PAN-STARRS1 DISTANT z > 5.6 QUASAR SURVEY: MORE THAN 100 QUASARS WITHIN THE FIRST GYR OF THE UNIVERSE

Bañados

Venemans

Decarli

et al. 2016

ApJS

337

282

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Luminous quasars at > z 5.6 can be studied in detail with the current generation of telescopes and provide us with unique information on the first gigayear of the universe. Thus far, these studies have been statistically limited by the number of quasars known at these redshifts. Such quasars are rare, and therefore, wide-field surveys are required to identify them, and multiwavelength data are required to separate them efficiently from their main contaminants, the far more numerous cool dwarfs. In this paper, we update and extend the selection for thez 6 quasars presented in Bañados et al. (2014) using the Pan-STARRS1 (PS1) survey. We present the PS1 distant quasar sample, which currently consists of 124 quasars in the redshift range   z 5.6 6.7 that satisfy our selection criteria. Of these quasars, 77 have been discovered with PS1, and 63 of them are newly identified in this paper. We present the composite spectra of the PS1 distant quasar sample. This sample spans a factor of ∼20 in luminosity and shows a variety of emission line properties. The number of quasars at > z 5.6 presented in this work almost doubles the previously known quasars at these redshifts, marking a transition phase from studies of individual sources to statistical studies of the high-redshift quasar population, which was impossible with earlier, smaller samples.

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“…We then took spectra of all the remaining promising candidates using VLT/FORS2 (Appenzeller et al 1998), P200/DBSP (Oke & Gunn 1982), MMT/Red Channel (Schmidt et al 1989), Magellan/FIRE (Simcoe et al 2008), and LBT/MODS (Pogge et al 2010) spectrographs. Standard techniques were used to reduce the data (see Venemans et al 2013;Bañados et al 2014Bañados et al , 2016Chen et al 2016).…”

Section: Imaging and Spectroscopic Confirmationmentioning

confidence: 99%

Physical Properties of 15 Quasars at z ≳ 6.5

Mazzucchelli

Bañados

Venemans

et al. 2017

ApJ

328

444

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Quasars are galaxies hosting accreting supermassive black holes; due to their brightness, they are unique probes of the early universe. To date, only a few quasars have been reported at (<800 Myr after the big bang). In this work, we present six additional quasars discovered using the Pan-STARRS1 survey. We use a sample of 15 quasars to perform a homogeneous and comprehensive analysis of this highest-redshift quasar population. We report four main results: (1) the majority of quasars show large blueshifts of the broad C iv λ1549 emission line compared to the systemic redshift of the quasars, with a median value ∼3× higher than a quasar sample at ; (2) we estimate the quasars’ black hole masses ( (0.3–5) × 109 M ⊙) via modeling of the Mg ii λ2798 emission line and rest-frame UV continuum and find that quasars at high redshift accrete their material (with ) at a rate comparable to a luminosity-matched sample at lower redshift, albeit with significant scatter (0.4 dex); (3) we recover no evolution of the Fe ii/Mg ii abundance ratio with cosmic time; and (4) we derive near-zone sizes and, together with measurements for quasars from recent work, confirm a shallow evolution of the decreasing quasar near-zone sizes with redshift. Finally, we present new millimeter observations of the [C ii] 158 μm emission line and underlying dust continuum from NOEMA for four quasars and provide new accurate redshifts and [C ii]/infrared luminosity estimates. The analysis presented here shows the large range of properties of the most distant quasars.

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The multi-object double spectrographs for the Large Binocular Telescope

Cited by 129 publications

References 0 publications

Spectroscopy of Ultra-diffuse Galaxies in the Coma Cluster

Spectroscopy of Ultra-diffuse Galaxies in the Coma Cluster

THE PAN-STARRS1 DISTANT z > 5.6 QUASAR SURVEY: MORE THAN 100 QUASARS WITHIN THE FIRST GYR OF THE UNIVERSE

Physical Properties of 15 Quasars at z ≳ 6.5

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