The Cosmic Origins Spectrograph: on-orbit instrument performance

Osterman, Steve; Green, J.; Froning, Cynthia S.; Béland, S.; Burgh, Eric B.; Penton, Steven V.; Delker, T.; Ebbets, Dennis; Sahnow, David J.; Bacinski, J.; Kimble, Randy A.; Andrews, John P.; Wilkinson, Erik; McPhate, Jason B.; Siegmund, Oswald H. W.; Ake, Thomas B.; Aloisi, Alessandra; Biagetti, C.; Diaz, R. I.; Dixon, W. V.; Friedman, S. D.; Ghavamian, Parviz; Goudfrooij, Paul; Hartig, G.; Keyes, C. D.; Lennon, D. J.; Massa, Derck; Niemi, Sami-Matias; Oliveira, Cristina; Osten, Rachel A.; Proffitt, Charles; Smith, T. E.; Soderblom, David R.

doi:10.1007/s10509-011-0699-5

Cited by 106 publications

(62 citation statements)

References 14 publications

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“…Simultaneous HST far-ultraviolet (FUV) spectra of PG 1211 +143 listed in Table 1 were obtained on 2015 April 12 and 14 over four observations (PID 13947, PI: Lee) using the Cosmic Origins Spectrograph (COS; Osterman et al 2011;Green et al 2012). We used grating G140L to cover the 912-2000 Å wavelength range.…”

Section: Uv Observationsmentioning

confidence: 99%

The Ultra-fast Outflow of the Quasar PG 1211+143 as Viewed by Time-averaged Chandra Grating Spectroscopy

Danehkar

Nowak

Lee

et al. 2018

ApJ

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We present a detailed X-ray spectral study of the quasar PG 1211+143 based on Chandra High Energy Transmission Grating Spectrometer (HETGS) observations collected in a multi-wavelength campaign with UV data using the Hubble Space Telescope Cosmic Origins Spectrograph (HST-COS) and radio bands using the Jansky Very Large Array (VLA). We constructed a multi-wavelength ionizing spectral energy distribution using these observations and archival infrared data to create XSTAR photoionization models specific to the PG 1211+143 flux behavior during the epoch of our observations. Our analysis of the Chandra-HETGS spectra yields complex absorption lines from H-like and He-like ions of Ne, Mg, and Si, which confirm the presence of an ultra-fast outflow (UFO) with a velocity of approximately −17,300 km s −1 (outflow redshift z out ∼ −0.0561) in the rest frame of PG 1211+143. This absorber is well described by an ionization parameter x~-log 2.9 erg s cm 1 and column density~-N log 21.5 cm H 2 . This corresponds to a stable region of the absorber's thermal stability curve, and furthermore its implied neutral hydrogen column is broadly consistent with a broad Lyα absorption line at a mean outflow velocity of approximately −16,980 km s −1 detected by our HST-COS observations. Our findings represent the first simultaneous detection of a UFO in both X-ray and UV observations. Our VLA observations provide evidence for an active jet in PG 1211+143, which may be connected to the X-ray and UV outflows; this possibility can be evaluated using very-long-baseline interferometric observations.

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Section: Uv Observationsmentioning

confidence: 99%

The Ultra-fast Outflow of the Quasar PG 1211+143 as Viewed by Time-averaged Chandra Grating Spectroscopy

Danehkar

Nowak

Lee

et al. 2018

ApJ

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“…The advent of the Cosmic Origins Spectrograph (COS; Green et al 2012;Osterman et al 2011) on the Hubble Space Telescope (HST) has allowed much fainter background target QSOs to be observed. This has facilitated detailed studies of the CGM by targeting fainter QSOs which are projected within the virial radius of a foreground galaxy.…”

Section: Introductionmentioning

confidence: 99%

CHARACTERIZING THE CIRCUMGALACTIC MEDIUM OF NEARBY GALAXIES WITHHST/COS ANDHST/STIS ABSORPTION-LINE SPECTROSCOPY

Stocke

Keeney

Danforth

et al. 2013

ApJ

282

518

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The circumgalactic medium (CGM) of late-type galaxies is characterized using UV spectroscopy of 11 targeted QSO/galaxy pairs at z 0.02 with the Hubble Space Telescope Cosmic Origins Spectrograph (COS) and ∼60 serendipitous absorber/galaxy pairs at z 0.2 with the Space Telescope Imaging Spectrograph. CGM warm cloud properties are derived, including volume filling factors of 3%-5%, cloud sizes of 0.1-30 kpc, masses of 10-10 8 M , and metallicities of ∼0.1-1 Z . Almost all warm CGM clouds within 0.5 R vir are metal-bearing and many have velocities consistent with being bound, "galactic fountain" clouds. For galaxies with L 0.1 L * , the total mass in these warm CGM clouds approaches 10 10 M , ∼10%-15% of the total baryons in massive spirals and comparable to the baryons in their parent galaxy disks. This leaves 50% of massive spiral-galaxy baryons "missing." Dwarfs (<0.1 L * ) have smaller area covering factors and warm CGM masses ( 5% baryon fraction), suggesting that many of their warm clouds escape. Constant warm cloud internal pressures as a function of impact parameter (P /k ∼ 10 cm −3 K) support the inference that previous COS detections of broad, shallow O vi and Lyα absorptions are of an extensive (∼400-600 kpc), hot (T ≈ 10 6 K), intra-cloud gas which is very massive ( 10 11 M ). While the warm CGM clouds cannot account for all the "missing baryons" in spirals, the hot intra-group gas can, and could account for ∼20% of the cosmic baryon census at z ∼ 0 if this hot gas is ubiquitous among spiral groups.

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“…We also present near-UV lines (above 200 nm) to facilitate a comparison with corresponding spectral measurements of interstellar organic materials (Kwok & Sanford 2008). Such experiments are designed to be carried out on the Cosmic Origins Spectrograph (COS) of the Hubble Space Telescope (Osterman et al 2011). The near-UV channel of COS shows a high sensitivity in the region between 200 and 300 nm where lines of hydrogenated protonated naphthalene and proflavine exist.…”

Section: R E S U Lt S a N D Discussionmentioning

confidence: 99%

Electronic absorption spectra of hydrogenated protonated naphthalene and proflavine

Bonaca¹,

Bilalbegović²

2011

Monthly Notices of the Royal Astronomical Society

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We study hydrogenated cations of two polycyclic hydrocarbon molecules as models of hydrogenated organic species that form in the interstellar medium. Optical spectra of the hydrogenated naphthalene cation Hn–C10H+8 for n= 1, 2 and 10, as well as the astrobiologically interesting hydrogenated proflavine cation Hn–C13H11N+3 for n= 1 and 14, are calculated. The pseudopotential time‐dependent density functional theory is used. It is found that the fully hydrogenated proflavine cation H14–C13H11N+3 shows a broad spectrum in which the positions of individual lines are almost lost. The positions, shapes and intensities of lines change in hydronaphthalene and hydroproflavine cations, showing that hydrogen additions induce substantially different optical spectra in comparison with base polycyclic hydrocarbon cations. One calculated line in the visible spectrum of H10–C10H+8 and one in the visible spectrum of H–C13H11N+3 are close to the measured diffuse interstellar bands. We also present the positions of near‐ultraviolet lines.

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The Cosmic Origins Spectrograph: on-orbit instrument performance

Cited by 106 publications

References 14 publications

The Ultra-fast Outflow of the Quasar PG 1211+143 as Viewed by Time-averaged Chandra Grating Spectroscopy

The Ultra-fast Outflow of the Quasar PG 1211+143 as Viewed by Time-averaged Chandra Grating Spectroscopy

CHARACTERIZING THE CIRCUMGALACTIC MEDIUM OF NEARBY GALAXIES WITHHST/COS ANDHST/STIS ABSORPTION-LINE SPECTROSCOPY

Electronic absorption spectra of hydrogenated protonated naphthalene and proflavine

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