Average [O II] nebular emission associated with Mg II absorbers: dependence on Fe II absorption

Joshi, Ravi; Srianand, R.; Petitjean, P.; Noterdaeme, P.

doi:10.1093/mnras/sty121

Cited by 16 publications

(13 citation statements)

References 59 publications

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“…The flux zero-level in the BOSS spectra is slightly above zero, especially in the blue part of the spectra where we have the DLA absorption (Joshi et al, 2018). These residual flux could falsely be interpreted as the detection of a NEL in the DLA trough.…”

Section: Zero-level Correction and Nel Detectionmentioning

confidence: 75%

Eclipsing damped Ly α systems in the Sloan Digital Sky Survey Data Release 12★

Fathivavsari

Petitjean

Jamialahmadi

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present the results of our automatic search for proximate damped Lyα absorption (PDLA) systems in the quasar spectra from the Sloan Digital Sky Survey Data Release 12. We constrain our search to those PDLAs lying within 1500 km s −1 from the quasar to make sure that the broad DLA absorption trough masks most of the strong Lyα emission from the broad line region (BLR) of the quasar. When the Lyα emission from the BLR is blocked by these so-called eclipsing DLAs, narrow Lyα emission from the host galaxy could be revealed as a narrow emission line (NEL) in the DLA trough. We define a statistical sample of 399 eclipsing DLAs with log N (H i) ≥ 21.10. We divide our statistical sample into three subsamples based on the strength of the NEL detected in the DLA trough. By studying the stacked spectra of these subsamples, we found that absorption from high ionization species are stronger in DLAs with stronger NEL in their absorption core. Moreover, absorption from the excited states of species like Si ii are also stronger in DLAs with stronger NEL. We also found no correlation between the luminosity of the Lyα NEL and the quasar luminosity. These observations are consistent with a scenario in which the DLAs with stronger NEL are denser and physically closer to the quasar. We propose that these eclipsing DLAs could be the product of the interaction between infalling and outflowing gas. High resolution spectroscopic observation would be needed to shed some light on the nature of these eclipsing DLAs.

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Section: Zero-level Correction and Nel Detectionmentioning

confidence: 75%

Eclipsing damped Ly α systems in the Sloan Digital Sky Survey Data Release 12★

Fathivavsari

Petitjean

Jamialahmadi

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…12 are exceptionally high compared with the literature (Joshi et al 2018;Rodríguez Hidalgo et al 2012). Systems selected in the SDSS by having R FeII MgII > 0.5 are found to probe lower impact parameters; moreover, there seems to be a distinction between absorbers associated with high or low SFR depending on whether this ratio is above or below 0.5, respectively (Noterdaeme et al 2010;Joshi et al 2018). Our particular experimental setup confirms this trend in the present host galaxy: the four closest positions to G1 show simultaneously the strongest [O ii] emission (Fig.…”

Section: Some Of the R Feiimentioning

confidence: 75%

Slicing the cool circumgalactic medium along the major axis of a star-forming galaxy at z = 0.7

López

Tejos

Barrientos

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present spatially-resolved echelle spectroscopy of an intervening Mg ii-Fe ii-Mg i absorption-line system detected at z abs = 0.73379 toward the giant gravitational arc PSZ1 G311. 65-18.48. The absorbing gas is associated to an inclined disk-like starforming galaxy, whose major axis is aligned with the two arc-segments reported here. We probe in absorption the galaxy's extended disk continuously, at ≈ 3 kpc sampling, from its inner region out to 15× the optical radius. We detect strong (W 2796 0 > 0.3Å) coherent absorption along 13 independent positions at impact parameters D = 0-29 kpc on one side of the galaxy, and no absorption at D = 28-57 kpc on the opposite side (all de-lensed distances at z abs ). We show that: (1) the gas distribution is anisotropic; (2) W 2796 0 , W 2600 0 , W 2852 0 , and the ratio W 2600 0 /W 2796 0 , all anti-correlate with D; (3) the W 2796 0-D relation is not cuspy and exhibits significantly less scatter than the quasar-absorber statistics; (4) the absorbing gas is co-rotating with the galaxy out to D 20 kpc, resembling a 'flat' rotation curve, but at D 20 kpc velocities decline below the expectations from a 3D disk-model extrapolated from the nebular [O ii] emission. These signatures constitute unambiguous evidence for rotating extra-planar diffuse gas, possibly also undergoing enriched accretion at its edge. Arguably, we are witnessing some of the long-sought processes of the baryon cycle in a single distant galaxy expected to be representative of such phenomena.

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“…Based on a study utilizing background galaxies to probe foreground galaxies, Rubin et al (2018) reported that W Mg II r is higher around galaxies with higher stellar mass and SFR, especially at R < 50 kpc. Further, using stacked spectra of background quasars, W Mg II r has been shown to be correlated with the [O II] luminosity surface density and hence the SFR (Noterdaeme, Srianand & Mohan 2010;Ménard et al 2011;Joshi et al 2018).…”

Section: Dependence Of Mg II Absorption On Galaxy Propertiesmentioning

confidence: 99%

MUSE Analysis of Gas around Galaxies (MAGG) – II: metal-enriched halo gas around z ∼ 1 galaxies

Dutta

Fumagalli

Fossati

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a study of the metal-enriched cool halo gas traced by Mg ii absorption around 228 galaxies at z ∼ 0.8 − 1.5 within 28 quasar fields from the MUSE Analysis of Gas around Galaxies (MAGG) survey. We observe no significant evolution in the Mg ii equivalent width versus impact parameter relation and in the Mg ii covering fraction compared to surveys at z ≲ 0.5. The stellar mass, along with distance from galaxy centre, appears to be the dominant factor influencing the Mg ii absorption around galaxies. With a sample that is 90% complete down to a star formation rate of ≈0.1 $\rm M_\odot yr^{-1}$PLXINSERT-, and up to impact parameters ≈250 − 350 kpc from quasars, we find that the majority ($67^{+12}_{-15}$% or 14/21) of the Mg ii absorption systems are associated with more than one galaxy. The complex distribution of metals in these richer environments adds substantial scatter to previously-reported correlations. Multiple galaxy associations show on average five times stronger absorption and three times higher covering fraction within twice the virial radius than isolated galaxies. The dependence of Mg ii absorption on galaxy properties disfavours the scenario in which a widespread intra-group medium dominates the observed absorption. This leaves instead gravitational interactions among group members or hydrodynamic interactions of the galaxy haloes with the intra-group medium as favoured mechanisms to explain the observed enhancement in the Mg ii absorption strength and cross section in rich environments.

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Average [O II] nebular emission associated with Mg II absorbers: dependence on Fe II absorption

Cited by 16 publications

References 59 publications

Eclipsing damped Ly α systems in the Sloan Digital Sky Survey Data Release 12★

Eclipsing damped Ly α systems in the Sloan Digital Sky Survey Data Release 12★

Slicing the cool circumgalactic medium along the major axis of a star-forming galaxy at z = 0.7

MUSE Analysis of Gas around Galaxies (MAGG) – II: metal-enriched halo gas around z ∼ 1 galaxies

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