OSIRIS tunable imager and spectrograph

Cepa, J.; Aguiar-González, M.; González-Escalera, V.; González‐Serrano, J. I.; Joven-Alvarez, Enrique; Cano, Lorenzo Peraza; Rasilla, J. L.; Rodríguez-Ramos, L. F.; González, Jesús; Duenas, Francisco J. Cobos; Sánchez, Beatríz; Tejada, Carlos; Bland-Hawthorn, J.; Militello, Carmelo; Rosa, F.

doi:10.1117/12.395520

Cited by 124 publications

(39 citation statements)

References 2 publications

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“…On 2014-07-22 we acquired 6 × 250 s of imaging in the rband with the Optical System for Imaging and low-IntermediateResolution Integrated Spectroscopy (OSIRIS; Cepa et al 2000) on the 10.4 m Gran Telescopio Canarias (GTC). We acquired imaging with the Low-Resolution Imaging Spectrograph (LRIS; Oke et al 1995) mounted at Keck, in the B, G, R, and RG 850 (similar to SDSS-z) filters on the nights of 2014-08-30 and 2014-08-31 (three exposures in each filter totaling between six and nine minutes total on-source).…”

Section: Late Time Imaging and Spectral Observationsmentioning

confidence: 99%

Gas inflow and outflow in an interacting high-redshift galaxy

Wiseman

Perley

Schady

et al. 2017

A&A

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We reveal multiple components of an interacting galaxy system at z ≈ 3.35 through a detailed analysis of the exquisite high-resolution Keck/HIRES spectrum of the afterglow of a gamma-ray burst (GRB). Through Voigt-profile fitting of absorption lines from the Lyman-series, we constrain the neutral hydrogen column density to N H i ≤ 10 18.35 cm −2 for the densest of four distinct systems at the host redshift of GRB 080810, among the lowest N H i ever observed in a GRB host, despite the line of sight passing within a projected 5 kpc of the galaxy centres. By detailed analysis of the corresponding metal absorption lines, we derive chemical, ionic and kinematic properties of the individual absorbing systems, and thus build a picture of the host as a whole. Striking differences between the systems imply that the line of sight passes through several phases of gas: the star-forming regions of the GRB host; enriched material in the form of a galactic outflow; the hot and ionised halo of a second, interacting galaxy falling towards the host at a line-of-sight velocity of 700 km s −1 ; and a cool, metal-poor cloud which may represent one of the best candidates yet for the inflow of metal-poor gas from the intergalactic medium.

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Section: Late Time Imaging and Spectral Observationsmentioning

confidence: 99%

Gas inflow and outflow in an interacting high-redshift galaxy

Wiseman

Perley

Schady

et al. 2017

A&A

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“…An X-ray source was detected with a count rate of 1. We obtained a spectrum with the OSIRIS instrument (Cepa et al 2000) on Gran Telescopio Canarias (GTC) in four 900s exposures with a mean epoch of 21.340 hr after the burst. We used the R1000B grism and a 1″ slit, with a resolution of R 1000.…”

Section: Grb 140808a/iptf14eagmentioning

confidence: 99%

THE NEEDLE IN THE 100 deg²HAYSTACK: UNCOVERING AFTERGLOWS OFFERMIGRBs WITH THE PALOMAR TRANSIENT FACTORY

Singer

Kasliwal

Cenko

et al. 2015

ApJ

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The Fermi Gamma-ray Space Telescope has greatly expanded the number and energy window of observations of gamma-ray bursts (GRBs). However, the coarse localizations of tens to a hundred square degrees provided by the Fermi GRB Monitor instrument have posed a formidable obstacle to locating the bursts' host galaxies, measuring their redshifts, and tracking their panchromatic afterglows. We have built a target-of-opportunity mode for the intermediate Palomar Transient Factory in order to perform targeted searches for Fermi afterglows. Here, we present the results of one year of this program: 8 afterglow discoveries out of 35 searches. Two of the bursts with detected afterglows (GRBs 130702A and 140606B) were at low redshift (z = 0.145 and 0.384, respectively) and had spectroscopically confirmed broad-line Type Ic supernovae. We present our broadband follow-up including spectroscopy as well as X-ray, UV, optical, millimeter, and radio observations. We study possible selection effects in the context of the total Fermi and Swift GRB samples. We identify one new outlier on the Amati relation. We find that two bursts are consistent with a mildly relativistic shock breaking out from the progenitor star rather than the ultra-relativistic internal shock mechanism that powers standard cosmological bursts. Finally, in the context of the Zwicky Transient Facility, we discuss how we will continue to expand this effort to find optical counterparts of binary neutron starmergers that may soon be detected by Advanced LIGO and Virgo.

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“…Images of P/2016 J1 have been obtained under photometric conditions on the nights of 14 May, 28 May, and 31 July, 2016. The images were obtained on a CCD using a Sloan r ′ filter in the Optical System for Image and Low Resolution Integrated Spectroscopy (OSIRIS) camera-spectrograph (Cepa et al 2000;Cepa 2010) at the GTC. The plate scale was 0.254 ′′ /pixel.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

The Splitting of Double-component Active Asteroid P/2016 J1 (PANSTARRS)

Moreno

Pozuelos

Novaković

et al. 2017

ApJL

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We present deep imaging observations, orbital dynamics, and dust tail model analyses of the double-component asteroid P/2016 J1 (J1-A and J1-B). The observations were acquired at the Gran Telescopio Canarias (GTC) and the CanadaFrance-Hawaii Telescope (CFHT) from mid March to late July, 2016. A statistical analysis of backward-in-time integrations of the orbits of a large sample of clone objects of P/2016 J1-A and J1-B shows that the minimum separation between them occurred most likely ∼2300 days prior to the current perihelion passage, i.e., during the previous orbit near perihelion. This closest approach was probably linked to a fragmentation event of their parent body. Monte Carlo dust tail models show that those two components became active simultaneously ∼250 days before the current perihelion, with comparable maximum loss rates of ∼0.7 kg s −1 and ∼0.5 kg s −1 , and total ejected masses of 8×10 6 kg and 6×10 6 kg for fragments J1-A and J1-B, respectively. In consequence, the fragmentation event and the present dust activity are unrelated. The simultaneous activation times -4 -of the two components and the fact that the activity lasted 6 to 9 months or longer, strongly indicate ice sublimation as the most likely mechanism involved in the dust emission process.

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OSIRIS tunable imager and spectrograph

Cited by 124 publications

References 2 publications

Gas inflow and outflow in an interacting high-redshift galaxy

Gas inflow and outflow in an interacting high-redshift galaxy

THE NEEDLE IN THE 100 deg²HAYSTACK: UNCOVERING AFTERGLOWS OFFERMIGRBs WITH THE PALOMAR TRANSIENT FACTORY

The Splitting of Double-component Active Asteroid P/2016 J1 (PANSTARRS)

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OSIRIS tunable imager and spectrograph

Cited by 124 publications

References 2 publications

Gas inflow and outflow in an interacting high-redshift galaxy

Gas inflow and outflow in an interacting high-redshift galaxy

THE NEEDLE IN THE 100 deg2HAYSTACK: UNCOVERING AFTERGLOWS OFFERMIGRBs WITH THE PALOMAR TRANSIENT FACTORY

The Splitting of Double-component Active Asteroid P/2016 J1 (PANSTARRS)

Contact Info

Product

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THE NEEDLE IN THE 100 deg²HAYSTACK: UNCOVERING AFTERGLOWS OFFERMIGRBs WITH THE PALOMAR TRANSIENT FACTORY