The UCSD/Keck Damped Lyα Abundance Database: A Decade of High‐Resolution Spectroscopy

Prochaska, J. Xavier; Wolfe, Arthur M.; Howk, J. C.; Gawiser, Eric; Burles, Scott; Cooke, Jeff

doi:10.1086/513714

Cited by 111 publications

(129 citation statements)

References 64 publications

(46 reference statements)

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“…In all comparisons for DLA absorption systems we used the nonrefractory element sulphur for metallicity estimation and for the determination of magnesium depletion because oxygen absorption lines are generally saturated (e.g. Prochaska et al 2007b). …”

Section: Comparison Of Magnesium Depletion In Objects Of Different Typesmentioning

confidence: 99%

“…Spectra of background sources allow us to probe regions of low-ionisation and cool gas present in the outer regions of spiral discs and dwarf irregular galaxies (Dessauges-Zavadsky et al 2004). Many Mg ii surveys have been carried out for these systems (Sargent et al 1988;Steidel & Sargent 1992;Dessauges-Zavadsky et al 2003;York et al 2006;Prochter et al 2006;Prochaska et al 2007b;Lilly et al 2007;Quider et al 2011). Owing to large spectroscopic surveys including the Sloan Digital Sky Survey (SDSS; York et al 2000) hundreds of thousands of quasars have been used to identify large samples of absorption systems along the line of sight using the Mg ii absorption lines (York et al 2006;Bouché et al 2006;Prochter et al 2006;Lundgren et al 2009;Quider et al 2011).…”

Section: Introductionmentioning

confidence: 99%

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The Mg IIλ2797,λ2803 emission in low-metallicity star-forming galaxies from the SDSS

Гусева

Izotov

Fricke

et al. 2013

A&A

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We present 65 Sloan Digital Sky Survey (SDSS) spectra of 62 star-forming galaxies with oxygen abundances 12 + log O/H ∼ 7.5-8.4.Redshifts of selected galaxies are in the range z ∼ 0.36-0.70. This allows us to detect the redshifted Mg ii λ2797, λ2803 emission lines. Our aim is to use these lines for the magnesium abundance determination. The Mg ii emission was detected in ∼2/3 of the galaxies. We find that the Mg ii λ2797 emission-line intensity follows a trend with the excitation parameter x = O 2+ /O that is similar to that predicted by CLOUDY photoionised H ii region models, suggesting a nebular origin of Mg ii emission. The Mg/O abundance ratio is lower by a factor ∼2 than the solar ratio. This is probably the combined effect of interstellar Mg ii absorption and depletion of Mg onto dust. However, the effect of dust depletion in selected galaxies, if present, is small, by a factor of ∼2 lower than that of iron.

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Section: Comparison Of Magnesium Depletion In Objects Of Different Typesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Mg IIλ2797,λ2803 emission in low-metallicity star-forming galaxies from the SDSS

Гусева

Izotov

Fricke

et al. 2013

A&A

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“…(2) The High Resolution Echelle Spectrograph (HIRES; Vogt et al 1994) located on the Keck I telescope on Mauna Kea, Hawaii. Our HIRES dataset is based on the sample published in Prochaska et al (2007), with several new QSO spectra taken from Wolfe et al (2008). The data reduction was conducted using the MAKEE package (developed and distributed by Barlow) for datasets taken with the original Tektronix CCD, and using the HIRedux package ) for data obtained with the newer CCD mosaic.…”

Section: Origin Of Datamentioning

confidence: 99%

Metal-enriched plasma in protogalactic halos

Fox¹,

Prochaska

Ledoux³

et al. 2009

A&A

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We continue our recent work of characterizing the plasma content of high-redshift damped and sub-damped Lyman-α systems (DLAs/sub-DLAs), which represent multi-phase gaseous (proto)galactic disks and halos seen toward a background source. We survey N v absorption in a sample of 91 DLAs and 18 sub-DLAs in the redshift range 1.67 < z abs < 4.28 with unblended coverage of the N v doublet. Our dataset includes high-resolution (6−8 km s are required to keep the cloud sizes physically reasonable. The nature of the remaining ≈80% of (broad) N v components is unclear; models of radiatively-cooling collisionally-ionized plasma at log (T /K) = 5.2−5.4 are fairly successful in reproducing the observed integrated high-ion column density ratios and the component line widths, but we cannot rule out photoionization by local sources.Finally, we identify several unusual DLAs with extremely low metallicity (<0.01 solar) but strong high-ion absorption (log N(N v) > 14 or log N(O vi) > 14.2), which present challenges to either galactic inflow or outflow models.

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“…The majority of the well-studied Damped Lyman-α systems (DLAs with logN(H i) ≥ 20.3) have lower metallicity and lower dust content than modern galaxies and presumably the more massive galaxies at z > 1 (e.g., Prochaska et al 2007;Rafelski et al 2012). 2DAs offer a unique opportunity to study the interstellar medium (ISM) of putatively evolved systems (at least chemically).…”

Section: Introductionmentioning

confidence: 99%

Quasar 2175 Å dust absorbers – II. Correlation analysis and relationship with other absorption line systems

Prochaska

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the cold neutral content (H i and C i gas) of 13 quasar 2175Å dust absorbers (2DAs) at z = 1.6 -2.5 to investigate the correlation between the presence of the UV extinction bump with other physical characteristics. These 2DAs were initially selected from the Sloan Digital Sky Surveys I -III and followed up with the Keck-II telescope and the Multiple Mirror Telescope as detailed in our Paper I. We perform a correlation analysis between metallicity, redshift, depletion level, velocity width, and explore relationships between 2DAs and other absorption line systems. The 2DAs on average have higher metallicity, higher depletion levels, and larger velocity widths than Damped Lyman-α absorbers (DLAs) or subDLAs. The correlation between [Zn/H] and [Fe/Zn] or [Zn/H] and log∆V 90 can be used as alternative stellar mass estimators based on the well-established mass-metallicity relation. The estimated stellar masses of the 2DAs in this sample are in the range of ∼ 10 9 to ∼2 × 10 11 M ⊙ with a median value of ∼2 × 10 10 M ⊙ . The relationship with other quasar absorption line systems can be described as (1) 2DAs are a subset of Mg ii and Fe ii absorbers, (2) 2DAs are preferentially metal-strong DLAs/subDLAs, (3) More importantly, all of the 2DAs show C i detections with logN(C i) > 14.0 cm −2 , (4) 2DAs can be used as molecular gas tracers. Their host galaxies are likely to be chemically enriched, evolved, massive (more massive than typical DLA/subDLA galaxies), and presumably star-forming galaxies.

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The UCSD/Keck Damped Lyα Abundance Database: A Decade of High‐Resolution Spectroscopy

Cited by 111 publications

References 64 publications

The Mg IIλ2797,λ2803 emission in low-metallicity star-forming galaxies from the SDSS

The Mg IIλ2797,λ2803 emission in low-metallicity star-forming galaxies from the SDSS

Metal-enriched plasma in protogalactic halos

Quasar 2175 Å dust absorbers – II. Correlation analysis and relationship with other absorption line systems

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