LUCIFER: a Multi-Mode NIR Instrument for the LBT

Seifert, W.; Appenzeller, I.; Baumeister, Harald; Bizenberger, Peter; Bomans, D. J.; Dettmar, R.‐J.; Grimm, Bernhard; Herbst, Tom; Hofmann, R.; Juette, M.; Laun, W.; Lehmitz, Michael; Lemke, R.; Lenzen, R.; Mandel, H.; Polsterer, Kai Lars; Rohloff, Ralf-Rainer; Schuetze, Andreas; Seltmann, Andreas; Thatte, Niranjan; Weiser, P.; Xu, Wei

doi:10.1117/12.459494

Cited by 79 publications

(33 citation statements)

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“…Since these observations are part of a program whose overall goal is to use difference imaging to characterize variable sources, the sub-images obtained for each epoch were not dithered and SN 2008S was always located at approximately the same point on Chip 2 of the cameras. Image exposure times were 300 s, generally with two exposures for U, B, and V and six exposures for R. The near-IR observations were made with LUCIFER (Seifert et al 2003;Mandel et al 2008; Ageorges et al 2010) in the H and K bands using the F3.75 camera with a pixel scale of 0. 12.…”

Section: Observations and Resultsmentioning

confidence: 99%

Dust to Dust: Three Years in the Evolution of the Unusual Sn 2008s

Szczygiel

Prieto²,

Kochanek

et al. 2012

ApJ

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We obtained late-time optical and near-IR imaging of SN 2008S with the Large Binocular Telescope, near-IR data with the Hubble Space Telescope, and mid-IR data with the Spitzer Space Telescope. We find that (1) it is again invisible at optical (UBVR) wavelengths to magnitude limits of approximately 25 mag, (2) while detected in the near-IR (H) at approximately 24.8 mag, it is fading rapidly, and (3) it is still brighter than the progenitor at 3.6 and 4.5 μm in the mid-IR with a slow, steady decline. The IR detections in 2010 December are consistent with dust emission at a blackbody temperature of T 640 K and a total luminosity of L 200,000 L , much higher than the L 40,000 L luminosity of the obscured progenitor star. The local environment also shows no evidence for stars significantly more massive than 10 M , consistent with the progenitor being an 8-10 M super asymptotic giant branch star.

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Section: Observations and Resultsmentioning

confidence: 99%

Dust to Dust: Three Years in the Evolution of the Unusual Sn 2008s

Szczygiel

Prieto²,

Kochanek

et al. 2012

ApJ

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“…We observed G15 1435+0110, L6-FLS 1712+6001, and NGP 1333+2357 with the LUCI-1 spectrograph (LBT NIRSpectroscopic Utility with Camera and Integral-Field Unit; Seifert et al 2003) on the Large Binocular Telescope (LBT) on 2015 April 14. We used the 200 l/mm H+K grating at λ c = 1.93 μm and the N1.8 camera (0 25 per pixel) to obtain a spectral range between 1.5 and 2.3 μm.…”

Section: Near-ir Spectroscopy Of the Vla-detected Smgsmentioning

confidence: 99%

The Circumgalactic Medium of Submillimeter Galaxies. I. First Results From a Radio-Identified Sample

Prochaska

Mutel

et al. 2016

ApJ

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We present the first results from an ongoing survey to characterize the circumgalactic medium (CGM) of massive high-redshift galaxies detected as submillimeter galaxies (SMGs). We constructed a parent sample of 163 SMG-QSO pairs with separations less than ∼36″ by cross-matching far-infrared-selected galaxies from Herschel with spectroscopically confirmed QSOs. The Herschel sources were selected to match the properties of the SMGs. We determined the sub-arcsecond positions of six Herschel sources with the Very Large Array and obtained secure redshift identification for three of those with near-infrared spectroscopy. The QSO sightlines probe transverse proper distances of 112, 157, and 198kpc at foreground redshifts of 2.043, 2.515, and 2.184, respectively, which are comparable to the virial radius of the ∼1013 M e halos expected to host SMGs. High-quality absorption-line spectroscopy of the QSOs reveals systematically strong H I Lyα absorption around all three SMGs, with rest-frame equivalent widths of ∼2-3Å. However, none of the three absorbers exhibit compelling evidence for optically thick H I gas or metal absorption, in contrast to the dominance of strong neutral absorbers in the CGM of luminous z∼2 QSOs. The low covering factor of optically thick H I gas around SMGs tentatively indicates that SMGs may not have as prominent cool gas reservoirs in their halos as the coeval QSOs and that they may inhabit less massive halos than previously thought.

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“…It is planned to build two identical instruments for both LBT mirrors having first light with LUCIFER 1 estimated in summer 2004. For more details see [1] and [5].…”

Section: Introductionmentioning

confidence: 98%

<title>LUCIFER control software: an OO approach using CORBA technology</title>

Jütte

Polsterer

Lehmitz³

et al. 2002

SPIE Proceedings

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In this paper we present the design of the control software for the LBT NIR spectroscopic Utility with Camera and Integral-Field Unit for Extragalactic Research (LUCIFER) which is one of the first-light instruments for the Large Binocular Telescope (LBT) on Mt. Graham, Arizona. The LBT will be equipped with two identical LUCIFER instruments for both mirrors. Furthermore we give an overview of the intended hardware structure of the instrument. Since the project requires a detailed and exact modeling of the software we present UML diagrams starting with an overall model down to use case, activity and class diagrams including an example for one special instrument unit.

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LUCIFER: a Multi-Mode NIR Instrument for the LBT

Cited by 79 publications

References 0 publications

Dust to Dust: Three Years in the Evolution of the Unusual Sn 2008s

Dust to Dust: Three Years in the Evolution of the Unusual Sn 2008s

The Circumgalactic Medium of Submillimeter Galaxies. I. First Results From a Radio-Identified Sample

<title>LUCIFER control software: an OO approach using CORBA technology</title>

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