First Light with RATIR: An Automated 6-band Optical/NIR Imaging Camera

Butler, Nathaniel R.; Klein, C. R.; Fox, O.; Lotkin, Gennadiy N.; Bloom, J.; Prochaska, J. Xavier; Ramírez-Ruiz, E.; Diego, J. A. de; Георгиев, Л.; González, J. Jesús; Lee, William H.; Richer, M. G.; Román, C. J.; Watson, A. M.; Gehrels, N.; Kutyrev, A.; Bernstein, R. A.; Alvarez, Luis; Ceseña, Urania; Clark, David M.; Colorado, E.; Córdova, Alejandro; Farah, Alejandro; García, B.; Guisa, G.; Herrera, Joel; Lazo, Francisco; López, Enrique Vera; Luna, Esther Martínez; Martı́nez, B.; Murillo, F.; Murillo, J.M.; Núñez, Juan; Pedrayes, María H.; Quirós, Fernando; Ochoa, José Luís; Sierra, Gerardo; Moseley, H.; Rapchun, David A.; Robinson, F. David; Samuel, Mathew V.; Sparr, Leroy

doi:10.1117/12.926471

Cited by 54 publications

(18 citation statements)

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“…Again, our pipeline software will be adapted from the software we have used since 2011 for RATIR. 6 Of course, it will require parallelization to handle approximately 288M pixels per minute in DDOTI rather than about 8M pixels per minute in RATIR. We will also modify the software to reject asteroids, known AGN, and flare stars, following iPTF.…”

Section: Pipeline Softwarementioning

confidence: 99%

DDOTI: the deca-degree optical transient imager

et al. 2016

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DDOTI will be a wide-field robotic imager consisting of six 28-cm telescopes with prime focus CCDs mounted on a common equatorial mount. Each telescope will have a field of view of 12 square degrees, will have 2 arcsec pixels, and will reach a 10-sigma limiting magnitude in 60 seconds of r = 18.7 in dark time and r = 18.0 in bright time. The set of six will provide an instantaneous field of view of about 72 square degrees. DDOTI uses commercial components almost entirely. The first DDOTI will be installed at the Observatorio Astron\'omico Nacional in Sierra San Pedro Mart\'ir, Baja California, M\'exico in early 2017. The main science goals of DDOTI are the localization of the optical transients associated with GRBs detected by the GBM instrument on the Fermi satellite and with gravitational-wave transients. DDOTI will also be used for studies of AGN and YSO variability and to determine the occurrence of hot Jupiters. The principal advantage of DDOTI compared to other similar projects is cost: a single DDOTI installation costs only about US$500,000. This makes it possible to contemplate a global network of DDOTI installations. Such geographic diversity would give earlier access and a higher localization rate. We are actively exploring this option.Comment: To appear in the proceedings of SPIE conference 9910 "Observatory Operations: Strategies, Processes, and Systems VI". 12 page

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Section: Pipeline Softwarementioning

confidence: 99%

DDOTI: the deca-degree optical transient imager

et al. 2016

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“…The instrumental magnitudes and colors of the SN were transformed to standard Johnson-Cousins BVRI using two stars in the SN field which are in the Sloan Digital Sky Survey (SDSS) catalog, and by following this prescription 12 to convert from the SDSS to the Johnson-Cousins system. Data in rizJH were also obtained with the multi-channel Reionization And Transients InfraRed camera (RATIR; Butler et al 2012) mounted on the 1.5 m Harold L. Johnson telescope at the Mexican Observatorio Astronómico Nacional on Sierra San Pedro Mártir in Baja California, Mexico. (Watson et al 2012).…”

Section: Early-time Photometrymentioning

confidence: 99%

THE TYPE IIb SUPERNOVA 2013df AND ITS COOL SUPERGIANT PROGENITOR

Dyk

Zheng

Fox

et al. 2014

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We have obtained early-time photometry and spectroscopy of supernova (SN) 2013df in NGC 4414. The SN is clearly of Type IIb, with notable similarities to SN 1993J. From its luminosity at secondary maximum light, it appears that less 56 Ni ( 0.06 M ) was synthesized in the SN 2013df explosion than was the case for the SNe IIb 1993J, 2008ax, and 2011dh. Based on a comparison of the light curves, the SN 2013df progenitor must have been more extended in radius prior to explosion than the progenitor of SN 1993J. The total extinction for SN 2013df is estimated to be A V = 0.30 mag. The metallicity at the SN location is likely to be solar. We have conducted Hubble Space Telescope (HST) Target of Opportunity observations of the SN with the Wide Field Camera 3, and from a precise comparison of these new observations to archival HST observations of the host galaxy obtained 14 yr prior to explosion, we have identified the progenitor of SN 2013df to be a yellow supergiant, somewhat hotter than a red supergiant progenitor for a normal Type II-Plateau SN. From its observed spectral energy distribution, assuming that the light is dominated by one star, the progenitor had effective temperature T eff = 4250 ± 100 K and a bolometric luminosity L bol = 10 4.94±0.06 L . This leads to an effective radius R eff = 545 ± 65 R . The star likely had an initial mass in the range of 13-17 M ; however, if it was a member of an interacting binary system, detailed modeling of the system is required to estimate this mass more accurately. The progenitor star of SN 2013df appears to have been relatively similar to the progenitor of SN 1993J.

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“…Where GROND (Greiner et al 2008) and RATIR (Butler et al 2012) have reported multicolor photometry in GCN circulars, we include their published data in Table 2 and our light-curve plots.…”

Section: Long-term Monitoring and Data Reductionmentioning

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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First Light with RATIR: An Automated 6-band Optical/NIR Imaging Camera

Cited by 54 publications

References 5 publications

DDOTI: the deca-degree optical transient imager

DDOTI: the deca-degree optical transient imager

THE TYPE IIb SUPERNOVA 2013df AND ITS COOL SUPERGIANT PROGENITOR

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

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First Light with RATIR: An Automated 6-band Optical/NIR Imaging Camera

Cited by 54 publications

References 5 publications

DDOTI: the deca-degree optical transient imager

DDOTI: the deca-degree optical transient imager

THE TYPE IIb SUPERNOVA 2013df AND ITS COOL SUPERGIANT PROGENITOR

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

Contact Info

Product

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