Performance and calibration of H2RG detectors and SIDECAR ASICs for the RATIR camera

Fox, O.; Kutyrev, A.; Rapchun, David A.; Klein, C.; Butler, Nathaniel R.; Bloom, J.; Diego, J. A. de; Farah, Alejandro; Gehrels, N.; Георгиев, Л.; González, J. Jesús; Lee, William H.; Loose, Markus; Lotkin, Gennadiy N.; Moseley, S. H.; Prochaska, J. X.; Ramírez-Ruiz, E.; Richer, M. G.; Robinson, F. David; Román-Zúñiga, C.; Samuel, Mathew V.; Sparr, Leroy; Watson, A. M.

doi:10.1117/12.926620

Cited by 22 publications

(13 citation statements)

References 11 publications

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“…The RC photometry was extracted using the automatic reference-subtraction photometry pipeline, FPipe (Fremling et al 2016), which utilizes reference images of the host galaxy from the Sloan Digital Sky Survey to subtract the background light. Additional photometry was obtained for iPTF17lf using the Reionization And Transients Infra-Red (RATIR; Fox et al 2012), camera mounted on the robotic 1.5 m Harold Johnson telescope of the Observatorio Astronómico Nacional. For the RATIR data, the SN and the host galaxy were fitted simultaneously by modeling the two using the point-spread function of the image and a Sérsic profile (Sérsic 1963).…”

Section: Spectroscopic Classification and Follow-upmentioning

confidence: 99%

iPTF Survey for Cool Transients

Adams

Blagorodnova

Kasliwal

et al. 2018

PASP

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We performed a wide-area (2000 deg 2 ) g and I band experiment as part of a two month extension to the Intermediate Palomar Transient Factory. We discovered 36 extragalactic transients including iPTF17lf, a highly reddened local SN Ia, iPTF17bkj, a new member of the rare class of transitional Ibn/IIn supernovae, and iPTF17be, a candidate luminous blue variable outburst. We do not detect any luminous red novae and place an upper limit on their rate. We show that adding a slow-cadence I band component to upcoming surveys such as the Zwicky Transient Facility will improve the photometric selection of cool and dusty transients.

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Section: Spectroscopic Classification and Follow-upmentioning

confidence: 99%

iPTF Survey for Cool Transients

Adams

Blagorodnova

Kasliwal

et al. 2018

PASP

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“…Some of the optical non-detections are consistent with an extrapolation from the X-ray emission using a standard unreddened synchrotron power-law spectrum. However, approximately 25-50 per cent require a steeper spectrum (Melandri et al 2008;Cenko et al 2009;Fynbo et al 2009;Greiner et al 2011;Melandri et al 2012), and these are called "optically dark" GRBs (Jakobsson et al 2004;Rol et al 2005;van der Horst et al 2009).…”

Section: )mentioning

confidence: 99%

“…RATIR is a six band simultaneous optical and NIR imager mounted on the autonomous 1.5 m Harold L. Johnson Telescope at the Observatorio Astronómico Nacional on Sierra San Pedro Mártir in Baja California, Mexico. Since commencing full operations in 2012 December, RATIR has been responding to GRB triggers from the Swift satellite, obtaining simultaneous photometry in the r, i, Z, Y, J and H bands (Butler et al 2012;Watson et al 2012;Klein et al 2012;Fox et al 2012).…”

Section: Ratir Datamentioning

confidence: 99%

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A detailed study of the optical attenuation of gamma-ray bursts in the Swift era

Littlejohns

Butler

Cucchiara

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present optical and near-infrared (NIR) photometry of 28 gamma-ray bursts (GRBs) detected by the Swift satellite and rapidly observed by the Reionization and Transients Infrared/Optical (RATIR) camera. We compare the optical flux at fiducial times of 5.5 and 11 hours after the high-energy trigger to that in the X-ray regime to quantify optical darkness. 46±9 per cent (13/28) of all bursts in our sample and 55±10 per cent (13/26) of long GRBs are optically dark, which is statistically consistently with previous studies. Fitting RATIR optical and NIR spectral energy distributions (SEDs) of 19 GRBs, most (6/7) optically dark GRBs either occur at high-redshift (z > 4.5) or have a high dust content in their host galaxies (A V > 0.3). Performing K-S tests, we compare the RATIR sample to those previously presented in the literature, finding our distributions of redshift, optical darkness, host dust extinction and X-ray derived column density to be consistent. The one reported discrepancy is with host galaxy dust content in the BAT6 sample, which appears inconsistent with our sample and other previous literature. Comparing X-ray derived host galaxy hydrogen column densities to host galaxy dust extinction, we find that GRBs tend to occur in host galaxies with a higher metal-to-dust ratio than our own Galaxy, more akin to the Large and Small Magellanic Clouds. Finally, to mitigate time evolution of optical darkness, we measure β OX,rest at a fixed rest frame time, t rest = 1.5 hours and fixed rest frame energies in the X-ray and optical regimes. Choosing to evaluate optical flux at λ rest = 0.25 µm, we remove high-redshift as a source of optical darkness, demonstrating that optical darkness must result from either high-redshift, dust content in the host galaxy along the GRB sight line, or a combination of the two.

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“…The lid of the box holds a 58.5x58.5x5.5mm filter/blank central to the optical axis. This design closely follows that of RATIR, 8 in that instead of potting the 15 ′′ flex cable connecting the (cold) SIDECAR and the (warm) JADE2 through the cryostat wall, the JADE2 is instead kept under vacuum inside the cryostat. In this configuration, both the power and data lines are connected to to a hermetically sealed MIL-Spec socket, with the data transferred externally over a multimode OM1 fibre optic cable to the instrument control computers (ICCs) located off the telescope.…”

Section: Introductionmentioning

confidence: 99%

IO:I, a near-infrared camera for the Liverpool Telescope

Barnsley

Jermak

Steele

et al. 2016

J. Astron. Telesc. Instrum. Syst

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IO:I is a new instrument that has recently been commissioned for the Liverpool Telescope, extending current imaging capabilities beyond the optical and into the near infrared. Cost has been minimised by use of a previously decommissioned instrument's cryostat as the base for a prototype and retrofitting it with Teledyne's 1.7µm cutoff Hawaii-2RG HgCdTe detector, SIDECAR ASIC controller and JADE2 interface card. In this paper, the mechanical, electronic and cryogenic aspects of the cryostat retrofitting process will be reviewed together with a description of the software/hardware setup. This is followed by a discussion of the results derived from characterisation tests, including measurements of read noise, conversion gain, full well depth and linearity. The paper closes with a brief overview of the autonomous data reduction process and the presentation of results from photometric testing conducted on on-sky, pipeline processed data.• Active Galactic Nuclei (AGN). Investigations into the variability of the various classes of AGN will allow us to probe the central engines of these objects, helping to discriminate between competing models.• Other areas of both time-domain (e.g. pixel microlensing, variability surveys) and non timedomain (e.g. metallicity gradients in galaxies and followup up X-ray cluster surveys) astronomy, proposals for which have already been solicited and undertaken. Instrument OverviewIO:I is positioned at the Cassegrain focus of the telescope where, without additional powered optics, the plate scale delivered at the focal plane is 97µm/ ′′ (2m diameter mirror, f/10 beam focal ratio). With a pixel pitch of 18µm, the total FOV of the 2048x2048 pixel detector is 6.27 ′ x6.27 ′ . The quantum efficiency of the detector is over 50% between 0.8 and 1.72 µm (peak 86% at 1.5µm), although the usable range within this window is limited by atmospheric transmission (see Figure 1). The detector itself is a HgCdTe Hawaii-2RG (H2RG) and is controlled via the SIDECAR ASIC controller and JADE2 interface card, all provided by Teledyne. Connected to the cryostat are two closed-cycle cooling units (IGC Polycold Cryotigers), each charged with PT13 gas, providing a total cooling capacity of 10W at a minimum temperature of 80K. Inside the cryostat are two corresponding cold heads. One of these cold heads is connected to the detector/SIDECAR mounting block. The other is attached to the floor of the radiation shield housing, shifting the bulk of the 300K blackbody radiative load incident from the warm cryostat chassis onto this thermal path. By thermally isolating the two paths, the majority of the cooling capacity provided by a single Cryotiger is available to cool the detector and SIDECAR only.Both J and H single filters have been procured, although the instrument has no filter wheel to allow robotic selection between the two. Following the requirements outlined by science proposals already received for this instrument, the H band filter has been preferred over the J. Changing between these various configurations is...

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Performance and calibration of H2RG detectors and SIDECAR ASICs for the RATIR camera

Cited by 22 publications

References 11 publications

iPTF Survey for Cool Transients

iPTF Survey for Cool Transients

A detailed study of the optical attenuation of gamma-ray bursts in the Swift era

IO:I, a near-infrared camera for the Liverpool Telescope

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