Atmospheric extinction properties above Mauna Kea from the Nearby SuperNova Factory spectro-photometric data set

Buton, C.; Copin, Y.; Aldering, G.; Antilogus, P.; Aragon, C.; Bailey, S.; Baltay, C.; Bongard, S.; Canto, A.; Cellier-Holzem, F.; Childress, M.; Chotard, N.; Fakhouri, H. K.; Gangler, É.; Guy, J.; Hsiao, E. Y.; Kerschhaggl, M.; Kowalski, M.; Loken, S.; Nugent, P.; Paech, K.; Pain, R.; Pécontal, É.; Pereira, R.; Perlmutter, S.; Rabinowitz, D.; Rigault, M.; Runge, K.; Scalzo, R.; Smadja, G.; Tao, C.; Thomas, R. C.; Weaver, B. A.; Wu, Chao

doi:10.1051/0004-6361/201219834

Cited by 93 publications

(96 citation statements)

References 45 publications

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“…The redshift z ≈ 0.091 was estimated from a weak narrow unresolved Hα emission, which seems to originate from the SN host galaxy. A line at λ ≈ 4675Å coincides with the HalfPower Point (HPP) between the red and the blue SNIFS channels (Buton et al 2013) redshifted to the iPTF13beo host redshift and shown in Figure 4. Therefore this line is probably an artifact produced by noise at the edges of the SNIFS channels.…”

Section: Spectroscopymentioning

confidence: 98%

“…The first one, referred to here as the 'early spectrum', was taken on 2013 May 21.594, ∼2.2 days after the first SN detection, ∼2.4 days after the estimated SN explosion date (phase: +2.4 days 3 ) and ∼0.3 days before the primary peak. The spectrum was obtained using the Supernova Integral Field Spectrogaph (SNIFS, Lantz et al 2004;Buton et al 2013) mounted on the University of Hawaii 2.2-meter telescope (88-inch, UH88).…”

Section: Spectroscopymentioning

confidence: 99%

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iPTF13beo: the double-peaked light curve of a Type Ibn supernova discovered shortly after explosion

Gorbikov

Gal‐Yam

Ofek

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present optical photometric and spectroscopic observations of the Type Ibn (SN 2006jc-like) supernova iPTF13beo. Detected by the intermediate Palomar Transient Factory ∼3 hours after the estimated first light, iPTF13beo is the youngest and the most distant (∼430 Mpc) Type Ibn event ever observed. The iPTF13beo light curve is consistent with light curves of other Type Ibn SNe and with light curves of fast Type Ic events, but with a slightly faster rise-time of two days. In addition, the iPTF13beo Rband light curve exhibits a double-peak structure separated by ∼9 days, not observed before in any Type Ibn SN. A low-resolution spectrum taken during the iPTF13beo rising stage is featureless, while a late-time spectrum obtained during the declining stage exhibits narrow and intermediate-width He I and Si II features with FWHM ≈ 2000-5000 km s −1 and is remarkably similar to the prototypical SN Ibn 2006jc spectrum. We suggest that our observations support a model of a massive star exploding in a dense He-rich circumstellar medium (CSM). A shock breakout in a CSM model requires an eruption releasing a total mass of ∼0.1 M⊙ over a time scale of couple of weeks prior to the SN explosion.

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Section: Spectroscopymentioning

confidence: 98%

Section: Spectroscopymentioning

confidence: 99%

iPTF13beo: the double-peaked light curve of a Type Ibn supernova discovered shortly after explosion

Gorbikov

Gal‐Yam

Ofek

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…The pipeline detailed in Bacon et al (2001) performs dark, bias, and flat-field corrections, cleans the data of bad pixels and cosmic rays, then fits and extracts the integral field unit spaxels into a one-dimensional spectrum. The Gaidos et al (2014) reduction takes this spectrum and performs flux calibration and telluric correction based on white dwarf standards taken throughout the night and a model of the atmosphere above Maunakea (Buton et al 2013). The final reduced spectrum of LSPMJ1314+1320AB has a signal-tonoise ratio (S/N) of >100 pixel −1 redward of 6000 Å.…”

Section: Uh22 M/supernova Integral Field Spectrograph (Snifs) and Imentioning

confidence: 99%

High-Precision Radio and Infrared Astrometry of LSPM J1314+1320ab. Ii. Testing Pre-Main-Sequence Models at the Lithium Depletion Boundary With Dynamical Masses

Dupuy

Forbrich

Rizzuto

et al. 2016

ApJ

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We present novel tests of pre-main-sequence models based on individual dynamical masses for the M7 binary LSPMJ1314+1320AB. Joint analysis of Keck adaptive optics astrometric monitoring along with Very Long Baseline Array radio data from a companion paper yield component masses of 92.8±0.6 M Jup (0.0885±0.0006 M ☉ ) and 91.7±1.0 M Jup (0.0875±0.0010 M ☉ ) and a parallactic distance of 17.249±0.013 pc. We find component luminosities consistent with the system being coeval at 80.8±2.5 Myr, according to BHAC15 evolutionary models. The presence of lithium is consistent with model predictions, marking the first test of the theoretical lithium depletion boundary using ultracool dwarfs of known mass. However, we find that the evolutionary model-derived average effective temperature (2950±5 K) is 180 K hotter than that given by a spectral type-T eff relation based on BT-Settl models (2770±100 K). We suggest that the dominant source of this discrepancy is model radii being too small by ≈13%. In a test mimicking the typical application of models by observers, we derive masses on the H-R diagram using luminosity and BT-Settl temperature. The estimated masses are lower by -(2.0σ) than we measure dynamically and would imply that this is a system of ≈50 M Jup brown dwarfs, highlighting the large systematic errors possible in H-R diagram properties. This is the first time masses have been measured for ultracool ( M6) dwarfs displaying spectral signatures of low gravity. Based on features in the infrared, LSPMJ1314+1320AB appears to have higher gravity than typical Pleiades and ABDor members, opposite the expectation given its younger age. The components of LSPMJ1314+1320AB are now the nearest, lowest mass pre-main-sequence stars with direct mass measurements.

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“…The flux calibration was developed in Sect. 2.2 of Pereira et al (2013), based on the atmospheric extinction derived in Buton et al (2013). The SNIFS data used in this paper are reduced according to the initial steps of SNIFS pipeline, e.g.…”

Section: Snifsmentioning

confidence: 99%

“…The advantage in calibrating SNIFS with such precision is that it is an integral field spectrograph (IFS), thus allowing us to produce spectrophotometric calibrated spectra of standard stars. These spectra are also corrected for the atmospheric extinction which is computed nightly from standard stars observations (Buton et al 2013). Therefore, the resulting physical calibration can be directly transferred to standard stars.…”

Section: Introductionmentioning

confidence: 99%

SCALA: In situ calibration for integral field spectrographs

Lombardo¹,

Küsters²,

Kowalski³

et al. 2017

A&A

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Aims. The scientific yield of current and future optical surveys is increasingly limited by systematic uncertainties in the flux calibration. This is the case for type Ia supernova (SN Ia) cosmology programs, where an improved calibration directly translates into improved cosmological constraints. Current methodology rests on models of stars. Here we aim to obtain flux calibration that is traceable to state-of-the-art detector-based calibration. Methods. We present the SNIFS Calibration Apparatus (SCALA), a color (relative) flux calibration system developed for the SuperNova integral field spectrograph (SNIFS), operating at the University of Hawaii 2.2 m (UH 88) telescope. Results. By comparing the color trend of the illumination generated by SCALA during two commissioning runs, and to previous laboratory measurements, we show that we can determine the light emitted by SCALA with a long-term repeatability better than 1%. We describe the calibration procedure necessary to control for system aging. We present measurements of the SNIFS throughput as estimated by SCALA observations. Conclusions. The SCALA calibration unit is now fully deployed at the UH 88 telescope, and with it color-calibration between 4000 Å and 9000 Å is stable at the percent level over a one-year baseline.

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Atmospheric extinction properties above Mauna Kea from the Nearby SuperNova Factory spectro-photometric data set

Cited by 93 publications

References 45 publications

iPTF13beo: the double-peaked light curve of a Type Ibn supernova discovered shortly after explosion

iPTF13beo: the double-peaked light curve of a Type Ibn supernova discovered shortly after explosion

High-Precision Radio and Infrared Astrometry of LSPM J1314+1320ab. Ii. Testing Pre-Main-Sequence Models at the Lithium Depletion Boundary With Dynamical Masses

SCALA: In situ calibration for integral field spectrographs

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