On-sky commissioning of Hamamatsu CCDs in GMOS-S

Gimeno, G.; Roth, Katherine C.; Chiboucas, Kristin; Hibon, Pascale; Boucher, Luc; White, J.K.; Rippa, Matthew; Labrie, Kathleen; Turner, James; Hanna, Kevin; Lazo, Manuel; Pérez, Gabriel; Rogers, Rolando; Rojas, R.G.; Placco, Vinicius M.; Murowinski, Richard

doi:10.1117/12.2233883

Cited by 61 publications

(21 citation statements)

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“…SN2016gkg was observed with the Gemini South telescope and the GMOS-S instrument (Hook et al 2004;Gimeno et al 2016), on 2017 August 20 and 26 (UT dates are used throughout). At the median date of observation, August 23, the phase corresponds to +320 days after light-curve maximum.…”

Section: Observations and Data Reductionsmentioning

confidence: 99%

Direct Evidence of Two-component Ejecta in Supernova 2016gkg from Nebular Spectroscopy*

Kuncarayakti

Folatelli

Maeda

et al. 2020

ApJ

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Spectral observations of the type-IIb supernova (SN) 2016gkg at 300-800 days are reported. The spectra show nebular characteristics, revealing emission from the progenitor star's metal-rich core and providing clues to the kinematics and physical conditions of the explosion. The nebular spectra are dominated by emission lines of [O I]λλ6300, 6364 and [Ca II]λλ7292, 7324. Other notable, albeit weaker, emission lines include MgI]λ4571, [Fe II]λ7155, OIλ7774, Ca II triplet, and a broad, boxy feature at the location of Hα. Unlike in other stripped-envelope SNe, the [O I] doublet is clearly resolved due to the presence of strong narrow components. The doublet shows an unprecedented emission line profile consisting of at least three components for each [O I]λ6300, 6364 line: a broad component (width ∼2000 km s −1), and a pair of narrow blue and red components (width ∼300 km s −1) mirrored against the rest velocity. The narrow component appears also in other lines, and is conspicuous in [O I]. This indicates the presence of multiple distinct kinematic components of material at low and high velocities. The low-velocity components are likely to be produced by a dense, slow-moving emitting region near the center, while the broad components are emitted over a larger volume. These observations suggest an asymmetric explosion, supporting the idea of two-component ejecta that influence the resulting late-time spectra and light curves. SN2016gkg thus presents striking evidence for significant asymmetry in a standard-energy SN explosion. The presence of material at low velocity, which is not predicted in 1D simulations, emphasizes the importance of multidimensional explosion modeling of SNe.

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Section: Observations and Data Reductionsmentioning

confidence: 99%

Direct Evidence of Two-component Ejecta in Supernova 2016gkg from Nebular Spectroscopy*

Kuncarayakti

Folatelli

Maeda

et al. 2020

ApJ

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“…We observed ESO601-G036 using the Gemini Multi-Object Spectrograph (GMOS; Hook et al 2004;Gimeno et al 2016) on Gemini-South on 2018 July11 UT. We used the B600 grating with a 0 75 wide slit oriented along its major axis for a total of 5 minutes exposure time with wavelength coverage of 3700-6850 Å and dispersion of ≈1 Å/pixel.…”

Section: Optical Follow-up Of Eso601-g036mentioning

confidence: 99%

A Search for the Host Galaxy of FRB 171020

Mahony

Ekers

Macquart

et al. 2018

ApJL

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We report on a search for the host galaxy of FRB171020, the fast radio burst (FRB) with the smallest recorded dispersion measure (DM; DM=114 pc cm −3) of our ongoing ASKAP survey. The low DM confines the burst location within a sufficiently small volume to rigorously constrain the identity of the host galaxy. We identify 16 candidate galaxies in the search volume and single out ESO601-G036, an Sc galaxy at redshift z=0.00867, as the most likely host galaxy. Ultraviolet and optical imaging and spectroscopy reveal that this galaxy has a star formation rate of approximately 0.1 M e yr −1 and oxygen abundance 12+log(O/H)=8.3±0.2, properties that are remarkably consistent with the galaxy hosting the repeating FRB121102. However, in contrast to FRB121102, follow-up radio observations of ESO601-G036 show no compact radio emission above a 5σ limit of L 2.1GHz =3.6×10 19 W Hz −1. Using radio continuum observations of the field, combined with archival optical imaging data, we find no analog to the persistent radio source associated with FRB121102 within the localization region of FRB171020 out to z=0.06. These results suggest that FRBs are not necessarily associated with a luminous and compact radio continuum source.

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“…We also obtained spectroscopy with the GMOS spectrographs (Hook et al 2004;Gimeno et al 2016) on both Gemini North and Gemini South 8.1 m telescopes. The exposures were taken with a 0.75" slit.…”

Section: Observationsmentioning

confidence: 99%

The sdA problem – II. Photometric and spectroscopic follow-up

Pelisoli

Koester

Castanheira

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Subdwarf A star (sdA) is a spectral classification given to objects showing H-rich spectra and sub-main sequence surface gravities, but effective temperature lower than the zero-age horizontal branch. Their evolutionary origin is an enigma. In this work, we discuss the results of follow-up observations of selected sdAs. We obtained time resolved spectroscopy for 24 objects, and time-series photometry for another 19 objects. For two targets, we report both spectroscopy and photometry observations. We confirm seven objects to be new extremely-low mass white dwarfs (ELMs), one of which is a known eclipsing star. We also find the eighth member of the pulsating ELM class.

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On-sky commissioning of Hamamatsu CCDs in GMOS-S

Cited by 61 publications

References 1 publication

Direct Evidence of Two-component Ejecta in Supernova 2016gkg from Nebular Spectroscopy*

Direct Evidence of Two-component Ejecta in Supernova 2016gkg from Nebular Spectroscopy*

A Search for the Host Galaxy of FRB 171020

The sdA problem – II. Photometric and spectroscopic follow-up

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