Automation of the OAN/SPM 1.5-meter Johnson telescope for operations with RATIR

Watson, A. M.; Richer, M. G.; Bloom, J.; Butler, Nathaniel R.; Ceseña, Urania; Clark, David M.; Colorado, E.; Córdova, Alejandro; Farah, Alejandro; Fox-Machado, L.; Fox, O.; García, B.; Георгиев, Л.; González, J. Jesús; Guisa, G.; Gutiérrez, L.; Herrera, Joel; Klein, C.; Kutyrev, A.; Lazo, Francisco; Lee, William H.; López, Enrique Vera; Luna, Esther Martínez; Martı́nez, B.; Murillo, F.; Murillo, J.M.; Núñez, Juan; Prochaska, J. X.; Ochoa, José Luís; Quirós, Fernando; Rapchun, David A.; Román-Zúñiga, C.; Valyavin, G. G.

doi:10.1117/12.926927

Cited by 36 publications

(10 citation statements)

References 13 publications

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“…Post-discovery, ground-based follow-up imaging in the optical and near-IR was also obtained for several SPIRITS transients. Near-IR JHK s -band images were obtained with the Multi-object Spectrometer for Infra-red Exploration (MOS-FIRE;McLean et al 2010McLean et al , 2012 (Watson et al 2012).…”

Section: 2mentioning

confidence: 99%

The SPIRITS Sample of Luminous Infrared Transients: Uncovering Hidden Supernovae and Dusty Stellar Outbursts in Nearby Galaxies*

Jencson

Kasliwal

Adams

et al. 2019

ApJ

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We present a systematic study of the most luminous (M IR [Vega magnitudes] brighter than −14) infrared (IR) transients discovered by the SPitzer InfraRed Intensive Transients Survey (SPIRITS) between 2014-2018 in nearby galaxies (D < 35 Mpc). The sample consists of 9 events that span peak IR luminosities of M [4.5],peak between −14 and −18.2, show IR colors between 0.2 < ([3.6] − [4.5]) < 3.0, and fade on timescales between 55 < t fade < 480 days. The two reddest events (A V > 12) show multiple, luminous IR outbursts over several years and have directly detected, massive progenitors in archival imaging. With analyses of extensive, multi-wavelength follow-up, we infer the following likely classifications: 5 obscured core-collapse supernovae (CCSNe), 2 erupting massive stars, 1 massive stellar merger, and 1 possible electron capture SN. We define a control sample of all optically discovered transients recovered in SPIRITS galaxies and satisfying the same selection criteria. The control sample consists of 8 core-collapse supernovae (CCSNe) and 1 Type Iax SN. We find that 7 of the 13 CCSNe in the SPIRITS sample have lower bounds on extinction of 2 < A V < 8, suggesting that a large population of CCSNe is heavily obscured. We estimate a nominal fraction of CCSNe in nearby galaxies that are missed by optical surveys of 38.5 +26.0 −21.9 % (90% confidence). This may resolve long-standing discrepancies between measurements of the CCSN rate and the cosmic star-formation rate.

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Section: 2mentioning

confidence: 99%

The SPIRITS Sample of Luminous Infrared Transients: Uncovering Hidden Supernovae and Dusty Stellar Outbursts in Nearby Galaxies*

Jencson

Kasliwal

Adams

et al. 2019

ApJ

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“…We also obtained rizY JH photometry of iPTF16geu (Watson et al 2012). The RATIR data were reduced and coadded using standard CCD and IR processing techniques in IDL and Python, utilizing the online astrometry programs SExtractor and SWarp.…”

Section: Ground Datamentioning

confidence: 99%

Magnification, dust and time-delay constraints from the first resolved strongly lensed Type Ia supernova iPTF16geu

Dhawan

Johansson

Goobar

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We report lensing magnifications, extinction, and time-delay estimates for the first resolved, multiply-imaged Type Ia supernova iPTF16geu, at z = 0.409, using Hubble Space Telescope (HST) observations in combination with supporting ground-based data. Multi-band photometry of the resolved images provides unique information about the differential dimming due to dust in the lensing galaxy. Using HST and Keck AO reference images taken after the SN faded, we obtain a total lensing magnification for iPTF16geu of µ = 67.8 +2.6 −2.9 , accounting for extinction in the host and lensing galaxy. As expected from the symmetry of the system, we measure very short time-delays for the three fainter images with respect to the brightest one: -0.23 ± 0.99, -1.43 ± 0.74 and 1.36 ± 1.07 days. Interestingly, we find large differences between the magnifications of the four supernova images, even after accounting for uncertainties in the extinction corrections: ∆m 1 = −3.88 +0.07 −0.06 , ∆m 2 = −2.99 +0.09 −0.08 , ∆m 3 = −2.19 +0.14 −0.15 and ∆m 4 = −2.40 +0.14 −0.12 mag, discrepant with model predictions suggesting similar image brightnesses. A possible explanation for the large differences is gravitational lensing by substructures, micro-or millilensing, in addition to the large scale lens causing the image separations. We find that the inferred magnification is insensitive to the assumptions about the dust properties in the host and lens galaxy.

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“…We obtained 18 epochs (days 7-76) of photometry of SN 2013fr using the multi-channel Reionization And Transients InfraRed camera (RATIR; Butler et al 2012) mounted on the 1.5 m Johnson telescope at the Mexican Observatorio Astronoḿico Nacional on Sierra San Pedro Mártir in Baja California, México (Watson et al 2012). Typical observations include a series of 80 s exposures in the ri bands and 60 s exposures in the ZY JH bands, with dithering between exposures.…”

Section: Ratir Photometrymentioning

confidence: 99%

SN 2013fs and SN 2013fr: exploring the circumstellar-material diversity in Type II supernovae

Bullivant

Smith

Williams

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present photometry and spectroscopy of SN 2013fs and SN 2013fr in the first ∼ 100 days post-explosion. Both objects showed transient, relatively narrow Hα emission lines characteristic of SNe IIn, but later resembled normal SNe II-P or SNe II-L, indicative of fleeting interaction with circumstellar material (CSM). SN 2013fs was discovered within 8 hr of explosion; one of the earliest SNe discovered thus far. Its light curve exhibits a plateau, with spectra revealing strong CSM interaction at early times. It is a less luminous version of the transitional SN IIn PTF11iqb, further demonstrating a continuum of CSM interaction intensity between SNe II-P and SNe IIn. It requires dense CSM within 6.5 × 10 14 cm of the progenitor, from a phase of advanced pre-SN mass loss beginning shortly before explosion. Spectropolarimetry of SN 2013fs shows little continuum polarization (∼ 0.5%, consistent with zero), but noticeable line polarization during the plateau phase. SN 2013fr morphed from a SN IIn at early times to a SN II-L. After the first epoch its narrow lines probably arose from host-galaxy emission, but the bright, narrow Hα emission at early times may be intrinsic to the SN. As for SN 2013fs, this would point to a short-lived phase of strong CSM interaction if proven to be intrinsic, suggesting a continuum between SNe IIn and SNe II-L. It is a low-velocity SN II-L like SN 2009kr, but more luminous. SN 2013fr also developed an infrared excess at later times, due to warm CSM dust that require a more sustained phase of strong pre-SN mass loss.

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Automation of the OAN/SPM 1.5-meter Johnson telescope for operations with RATIR

Cited by 36 publications

References 13 publications

The SPIRITS Sample of Luminous Infrared Transients: Uncovering Hidden Supernovae and Dusty Stellar Outbursts in Nearby Galaxies*

The SPIRITS Sample of Luminous Infrared Transients: Uncovering Hidden Supernovae and Dusty Stellar Outbursts in Nearby Galaxies*

Magnification, dust and time-delay constraints from the first resolved strongly lensed Type Ia supernova iPTF16geu

SN 2013fs and SN 2013fr: exploring the circumstellar-material diversity in Type II supernovae

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