An Efficient Low Resolution and Moderate Resolution Spectrograph for the Hale Telescope

Oke, J. B.; Gunn, J. E.

doi:10.1086/131027

Cited by 395 publications

(271 citation statements)

References 3 publications

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“…The spectrum was obtained using the Double Spectrograph (DBSP, Oke & Gunn 1982) The early spectrum is blue and is characterized by an absence of narrow or intermediate-width strong features. The redshift z ≈ 0.091 was estimated from a weak narrow unresolved Hα emission, which seems to originate from the SN host galaxy.…”

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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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: 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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“…Low-resolution spectroscopy from 0.3 to 1.0 m was obtained using the Double Spectrograph at the 5 m Hale Telescope (Oke & Gunn 1982) at Palomar Observatory, and spectroscopy from 1 to 2.5 m was obtained using NIRC ( Matthews & Soifer 1994), the facility near-infrared camera and spectrograph at the Keck Observatory. Visible photometry was obtained at the 1.3 m SMARTS telescope, while J and K s photometry was obtained with NIRC.…”

Section: Low-resolution Spectroscopymentioning

confidence: 99%

Methane and Ethane on the Bright Kuiper Belt Object 2005 FY9

et al. 2006

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The spectrum of the bright Kuiper Belt object 2005 FY9 from 0.34 to 2.5 m is dominated by the red coloring of many outer solar system objects in the optical wavelength regime and by absorption due to methane in the near-infrared. The solid methane absorption lines are significantly broader on 2005 FY9 than on any other solar system body, indicating long optical path lengths through the methane. These long path lengths can be parameterized as a methane grain size of approximately 1 cm in a Hapke reflectance model. In addition to large-grained methane, the infrared spectrum also indicates the clear presence of ethane, an expected product of UV photolysis of methane. No evidence for N 2 or CO, both known to be present on Pluto, is found. We suggest that the large differences between the spectrum of 2005 FY9 and that of Pluto and 2003 UB313 is due to a depletion of nitrogen on the surface of 2005 FY9 that leads to large methane grains, abundant sites for ethane formation through UV photolysis, and highly irradiated tholin-like material.

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“…A total of 18 spectra of HE 0024À2523 have been collected during several runs using three different instrumenttelescope combinations: UVES at VLT-UT2 Kueyen (Dekker et al 2000), HIRES at Keck I (Vogt et al 1994), and the double spectrograph at the Hale 5 m telescope at Palomar Mountain (Oke & Gunn 1982).…”

Section: Observations and Data Reductionsmentioning

confidence: 99%

Stellar Archaeology: A Keck Pilot Program on Extremely Metal-Poor Stars From the Hamburg/ESO Survey. III. The Lead (P[CLC]b[/CLC]) Star HE 0024−2523

Lucatello

Gratton

Cohen

et al. 2003

The Astronomical Journal

129

147

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We present a detailed abundance analysis, including spectral syntheses, of a very metal-poor ([Fe/H] ' À2.7) peculiar main-sequence star (HE 0024À2523) detected during the course of the Keck Pilot Program. Radial velocities of this star were obtained during four different observing runs over a time span of 1.1 yr and demonstrate that it is clearly a short-period spectroscopic binary. An orbital solution was obtained, and orbital parameters were determined with high precision. The rotational velocity was also measured (v rot sin i = 9.7 AE 1.5 km s À1 ); rotation appears likely to be synchronous with the orbit. The abundance analysis and spectral syntheses indicate that the object is a CH star characterized by extreme s-process enrichment, likely due to mass accretion from an evolved companion that has now probably become a white dwarf. The lead (Pb) abundance of (HE 0024À2523) is very high, the same as that of the recently discovered lead-rich, metal-poor star CS 29526-110, [Pb/Fe] = +3.3. The abundance ratio of the heavy to light s-elements, as characterized by Pb and Ba, [Pb/Ba] = +1.9, is the highest yet found for any metal-poor star and is about 0.7 dex higher than that of CS 29526-110. On the basis of the measured isotopic ratio of carbon (C 12 /C 13 $ 6) we argue that the mass donor must have had an original mass of at least $3 M . The unusually short period of this CH star suggests that it underwent a past common-envelope phase with its evolved companion. Our results are compared with the latest available models for asymptotic giant branch yields and s-process nucleosynthesis. We also discuss the possible connection between HE 0024À2523, the lithium depletion of halo stars, and halo blue straggler formation.

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An Efficient Low Resolution and Moderate Resolution Spectrograph for the Hale Telescope

Cited by 395 publications

References 3 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

Methane and Ethane on the Bright Kuiper Belt Object 2005 FY9

Stellar Archaeology: A Keck Pilot Program on Extremely Metal-Poor Stars From the Hamburg/ESO Survey. III. The Lead (P[CLC]b[/CLC]) Star HE 0024−2523

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