KOSMOS and COSMOS: new facility instruments for the NOAO 4-meter telescopes

Martini, Paul; Elias, J. H.; Points, Sean; Sprayberry, David; Derwent, Mark; Gonzàlez, R.; Mason, Jerry; O’Brien, T. P.; Pappalardo, Daniel; Pogge, Richard W.; Stoll, R.; Zhelem, Ross; Daly, Phil; Fitzpatrick, Mike; George, J. Richard; Hunten, Mark; Marshall, Robert; Poczulp, Gary; Rath, Susan A.; Seaman, R.; Trueblood, Mark; Zelaya, K.

doi:10.1117/12.2056834

Cited by 18 publications

(6 citation statements)

References 4 publications

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“…We used the EFOSC-2 (ESO Faint Object Spectrograph and Camera v.2; Buzzoni et al 1984) instrument with Grism#7 (600 gr mm −1 ) and a 1 0 slit, resulting in a wavelength coverage in the range [3300:5100] Å at resolving power R∼1200. KPNO Mayall Telescope-73 stars were observed with the 4 m Mayall telescope, located at Kitt Peak National Observatory, using the KOSMOS (Kitt Peak Ohio State Multi-Object Spectrograph; Martini et al 2014) instrument. We used the 600lmm −1 grating, the blue setting, and a 0 9 slit, resulting in a wavelength coverage in the range [3600:6300] Å at resolving power R∼1800.…”

Section: Medium-resolution Follow-up Observationsmentioning

confidence: 99%

The R-Process Alliance: Spectroscopic Follow-up of Low-metallicity Star Candidates from the Best & Brightest Survey

Placco

Santucci

Beers

et al. 2019

ApJ

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We present results from an observing campaign to identify low-metallicity stars in the Best & Brightest Survey. From medium-resolution (R ∼ 1, 200 − 2, 000) spectroscopy of 857 candidates, we estimate the stellar atmospheric parameters (T eff , log g, and [Fe/H]), as well as carbon and α-element abundances. We find that 69% of the observed stars have [Fe/H] ≤ −1.0, 39% have [Fe/H] ≤ −2.0, and 2% have [Fe/H] ≤ −3.0. There are also 133 carbon-enhanced metal-poor (CEMP) stars in this sample, with 97 CEMP Group I and 36 CEMP Group II stars identified in the A(C) versus [Fe/H] diagram. A subset of the confirmed low-metallicity stars were followed-up with high-resolution spectroscopy, as part of the R-process Alliance, with the goal of identifying new highly and moderately r-processenhanced stars. Comparison between the stellar atmospheric parameters estimated in this work and from high-resolution spectroscopy exhibit good agreement, confirming our expectation that mediumresolution observing campaigns are an effective way of selecting interesting stars for further, more targeted, efforts.

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Section: Medium-resolution Follow-up Observationsmentioning

confidence: 99%

The R-Process Alliance: Spectroscopic Follow-up of Low-metallicity Star Candidates from the Best & Brightest Survey

Placco

Santucci

Beers

et al. 2019

ApJ

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“…We obtained single epoch g-, r-, and i-band photometry for KISS15s with the Mayall 4-m Telescope in KOS-MOS imaging mode (Martini et al 2014) on 2017 July 25 UT (MJD=57959.5). KOSMOS was used with a 2k4k E2V charge-coupled device (CCD) with a pixel scale of 0 .292 pixel −1 .…”

Section: Mayall 4-m/kosmos Optical Photometrymentioning

confidence: 99%

A Long-duration Luminous Type IIn Supernova KISS15s: Strong Recombination Lines from the Inhomogeneous Ejecta–CSM Interaction Region and Hot Dust Emission from Newly Formed Dust*

Kokubo

Mitsuda

Morokuma

et al. 2019

ApJ

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We report the discovery of an SN 1988Z-like type IIn supernova KISS15s found in a low-mass star-forming galaxy at redshift z = 0.038 during the course of the Kiso Supernova Survey (KISS). KISS15s shows longduration optical continuum and emission line light curves, indicating that KISS15s is powered by a continuous interaction between the expanding ejecta and dense circumstellar medium (CSM). The Hα emission line profile can be decomposed into four Gaussians of narrow, intermediate, blue-shifted intermediate, and broad velocity width components, with a full width at half maximum of 100, ∼ 2, 000, and ∼ 14, 000 km s −1 for the narrow, intermediate, and broad components, respectively. The presence of the blue-shifted intermediate component, of which the line-of-sight velocity relative to the systemic velocity is about −5, 000 km s −1 , suggests that the ejecta-CSM interaction region has an inhomogeneous morphology and anisotropic expansion velocity. We found that KISS15s shows increasing infrared continuum emission, which can be interpreted as hot dust thermal emission of T ∼ 1, 200 K from newly formed dust in a cool, dense shell in the ejecta-CSM interaction region. The progenitor mass-loss rate, inferred from bolometric luminosity, isṀ ∼ 0.4 M yr −1 (v w /40 km s −1 ), where v w is the progenitor's stellar wind velocity. This implies that the progenitor of KISS15s was a red supergiant star or a luminous blue variable that had experienced a large mass-loss in the centuries before the explosion.

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“…comm. ), COSMOS (Martini et al 2014), Binospec (Fabricant et al 2019), X-Shooter (Vernet et al 2011), DBSP (Oke & Gunn 1982), EFOSC2, which is part of PESSTO (Smartt et al 2015), SNIFS (Lantz et al 2004;Lombardo et al 2017), and SEDM (Blagorodnova et al 2018). Figure supplied by E. Kirby.…”

Section: Spectroscopic Facilitiesmentioning

confidence: 99%

Towards An Integrated Optical Transient Utility

Kulkarni¹

2020

Preprint

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The ongoing optical time-domain astronomy surveys are routinely reporting fifty transient candidates per night. Here, I investigate the demographics of astronomical transients and supernova classifications reported to the Transient Name Server in the year 2019. I find that only a tenth of the transients were spectrally classified. This severe "bottleneck" problem should concern astronomers and also funding agencies. The bottleneck will get worse by a factor of 20 (or more) once LSST comes on line. We need to fundamentally rethink the purpose of surveys for transients. Here, after undertaking a detailed investigation of this issue I offer some solutions. Going forward, astronomers will employ two different methodologies: (1) multi-band photometric method which is well suited to the study of very large, many tens of thousands, samples of faint transients; (2) spectral classifications of thousands of bright transients found in shallow and nightly cadenced wide-field photometry surveys and transients associated with galaxies in the local Universe. The latter program, in addition to unearthing new types of transients and offering astronomers opportunities to undertake extensive follow up of interesting transients, is needed to set the stage for the former. Specifically, I suggest a globally coordinated effort to spectrally classify a complete sample of bright supernovae ( 19.5 mag) and transients within the local Universe (< 200 Mpc). The proposed program is within reach -thanks to the on-going widefield surveys, the development of novel spectrographs tuned for classification, great improvements in throughput of spectrographs and the increasing availability of robotic telescopes.

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KOSMOS and COSMOS: new facility instruments for the NOAO 4-meter telescopes

Cited by 18 publications

References 4 publications

The R-Process Alliance: Spectroscopic Follow-up of Low-metallicity Star Candidates from the Best & Brightest Survey

The R-Process Alliance: Spectroscopic Follow-up of Low-metallicity Star Candidates from the Best & Brightest Survey

A Long-duration Luminous Type IIn Supernova KISS15s: Strong Recombination Lines from the Inhomogeneous Ejecta–CSM Interaction Region and Hot Dust Emission from Newly Formed Dust*

Towards An Integrated Optical Transient Utility

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