On the observed - correlation in Sloan Digital Sky Survey QSO spectra

López, G.; Chen, Hsiao‐Wen

doi:10.1111/j.1365-2966.2011.19998.x

Cited by 21 publications

(23 citation statements)

References 33 publications

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“…This is what one expects based on the known W2796 versus ρ anti-correlation. While what we observe is consistent with the trend presented by López & Chen (2012) the actual detection fraction we find is much less than their model prediction because of the high luminosity threshold (i.e., 0.3L ⋆ [O II] ) imposed in our study. Here, we also find, for a given luminosity threshold, the [O ii] detection rate in Mg ii systems is higher in the SDSS-DR7 spectra than in the SDSS-DR12 spectra (see Fig.…”

Section: Detection Probability Of Nebular Emission Lines In Strong Mgsupporting

confidence: 78%

“…This is expected from the increasing projected area of fibre with z which leads to high probability for the line emitting regions to come inside the fibre. Interestingly, in an effort to model the effect of finite fibre size López & Chen (2012) have shown that the fraction of systems for which the absorbing galaxy will give rise to [O ii] emission in QSO spectra increases as a function of W2796 and will depend on the fibre size. They showed that the detection fraction increases from ∼50% for W2796> 1Å to ∼90% for W2796 > 3Å when no limiting flux condition is applied.…”

Section: Detection Probability Of Nebular Emission Lines In Strong Mgmentioning

confidence: 99%

“…This relationship is also found to be evolving with redshift in the sense that a given W2796 seems to be associated with larger Σ [O II] at high-z compared to that at low-z. Ménard et al (2011) have suggested that the Mg ii absorbers can in principle provide a new probe of the redshift evolution of the star formation rate density in a luminosity unbiased manner (however, see López & Chen 2012). Increasing the number of direct detections over a large redshift range will allow us to address this more efficiently.…”

Section: Introductionmentioning

confidence: 99%

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[O ii] nebular emission from Mg ii absorbers: star formation associated with the absorbing gas

Joshi

Srianand

Petitjean

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present nebular emission associated with 198 strong Mg ii absorbers at 0.35 z 1.1 in the fibre spectra of quasars from the Sloan Digital Sky Survey. Measured and their z evolution are consistent with those of galaxies detected in deep surveys. Based on the median stacked spectra, we infer the average metallicity (log Z ∼8.3), ionization parameter (log q ∼7.5) and stellar mass (log (M/M ⊙ )∼9.3). The Mg ii systems with nebular emission typically have W 2796 2Å, Mg ii doublet ratio close to 1 and W(Fe iiλ2600)/W 2796 ∼ 0.5 as often seen in damped Lyα and 21-cm absorbers at these redshifts. This is the biggest reported sample of [O ii] emission from Mg ii absorbers at low impact parameters ideally suited for probing various feedback processes at play in z 1 galaxies.

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Section: Detection Probability Of Nebular Emission Lines In Strong Mgsupporting

confidence: 78%

Section: Detection Probability Of Nebular Emission Lines In Strong Mgmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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[O ii] nebular emission from Mg ii absorbers: star formation associated with the absorbing gas

Joshi

Srianand

Petitjean

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…While this correlation does not necessarily imply the presence of winds (see López & Chen 2012), Nestor et al (2011) observed an association between the most extreme absorbers and starburst galaxies. These authors further showed that galactic outflows are necessary to account for the large velocity spread.…”

Section: Spatial Configuration and Massmentioning

confidence: 99%

Discovery of a compact gas-rich damped Lyman-αgalaxy atz = 2.2: evidence of a starburst-driven outflow

Noterdaeme

Laursen

Petitjean

et al. 2012

A&A

125

144

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We present the detection of Ly α, [O iii], and H α emission associated with an extremely strong damped Lyman-α (DLA) system (N(H i) = 10 22.10 cm −2 ) at z = 2.207 towards the quasar SDSS J113520.39−001053.56. This is the largest H i column density ever measured along a quasi-stellar object (QSO) line of sight, though typical of those often found in DLAs associated to gamma-ray bursts (GRBs). This absorption system can also be classified as an ultra-strong Mg ii system with W λ2796 , and is unresolved. From the H α line, we measure a significant star formation rate (SFR) ≈ 25 M yr −1 (uncorrected for dust). The shape of the Ly α line is double-peaked, which is the signature of a resonant scattering of Ly α photons, and the Ly α emission is spatially extended. More strikingly, the blue and red Ly α peaks arise from distinct regions extended over a few kpc on either side of the star-forming region. We propose that this is the consequence of a Ly α transfer in outflowing gas. The presence of starburst-driven outflows is also in agreement with the high SFR together with the small size and low mass of the galaxy (M vir ∼ 10 10 M ). By placing constraints on the stellar UV continuum luminosity of the galaxy, we estimate an age of at most a few 10 7 yr, again consistent with a recent starburst scenario. We interpret these data as the observation of a young, gas-rich, compact starburst galaxy, from which material is expelled through collimated winds powered by the vigorous star formation activity. We substantiate this picture by modelling the radiative transfer of Ly α photons in the galactic counterpart. Though our model (a spherical galaxy with bipolar outflowing jets) is a simplistic representation of the true gas distribution and velocity field, the agreement between the observed and simulated properties is particularly good (spectral shape and width of the Lyman-α emission, spatial configuration, escape fraction as well as absorption kinematics, H i column density, and dust reddening). Finally, we propose that selecting DLAs with very high H i column densities may be an efficient way of detecting star-forming galaxies at small impact parameters from the background QSO lines of sight.

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“…The authors find that the association between strong MgII and damped Lyman-α systems (DLAs) strengthens at higher redshifts, even though the overall taxonomy of these absorbers as defined in Churchill et al (2000) does not change. There is evidence that the redshift evolution in the number density of MgII absorbers follows the cosmic star formation rate (Zhu & Ménard 2012;Matejek & Simcoe 2012), though the A&A 552, A143 (2013) effects of observational bias may still play an important role (López & Chen 2012). Prochter et al (2006) compared the incidence of strong MgII absorbers in quasar sight-lines with those found in GRB afterglows.…”

Section: Introductionmentioning

confidence: 99%

Clustering of galaxies around gamma-ray burst sight-lines

Sudilovsky¹,

Greiner²,

Rau³

et al. 2013

A&A

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There is evidence of an overdensity of strong intervening MgII absorption line systems distributed along the lines of sight toward gamma-ray burst (GRB) afterglows relative to quasar sight-lines. If this excess is real, one should also expect an overdensity of field galaxies around GRB sight-lines, as strong MgII tends to trace these sources. In this work, we test this expectation by calculating the two point angular correlation function of galaxies within 120 (∼470 h −1 71 Kpc at z ∼ 0.4) of GRB afterglows. We compare the gamma-ray burst optical and near-infrared detector (GROND) GRB afterglow sample -one of the largest and most homogeneous samples of GRB fields -with galaxies and active galactic nuclei found in the COSMOS-30 photometric catalog. We find no significant signal of anomalous clustering of galaxies at an estimated median redshift of z ∼ 0.3 around GRB sight-lines, down to K AB < 19.3. This result is contrary to the expectations from the MgII excess derived from GRB afterglow spectroscopy, although many confirmed galaxy counterparts to MgII absorbers may be too faint to detect in our sample -especially those at z > 1. We note that the addition of higher sensitivity Spitzer/IRAC or HST/WFC3 data for even a subset of our sample would increase this survey's depth by several orders of magnitude, simultaneously increasing statistics and enabling the investigation of a much larger redshift space.

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On the observed - correlation in Sloan Digital Sky Survey QSO spectra

Cited by 21 publications

References 33 publications

[O ii] nebular emission from Mg ii absorbers: star formation associated with the absorbing gas

[O ii] nebular emission from Mg ii absorbers: star formation associated with the absorbing gas

Discovery of a compact gas-rich damped Lyman-αgalaxy atz = 2.2: evidence of a starburst-driven outflow

Clustering of galaxies around gamma-ray burst sight-lines

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