Large-scale structure in absorption: gas within and around galaxy voids

Tejos, Nicolás; Morris, Simon L.; Crighton, Neil H. M.; Theuns, Tom; Altay, Gabriel; Finn, Charles W.

doi:10.1111/j.1365-2966.2012.21448.x

Cited by 33 publications

(53 citation statements)

References 97 publications

(200 reference statements)

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“…Another aspect of voids that we did not measure, but would also be sensitive to matter density profiles, is the velocity field within voids; perhaps very faint tracers such as absorption lines can be used to constrain these (e.g. Tejos et al 2012). Another possible direction to constrain WDM is through the properties of filaments and perhaps walls in WDM, which we quantitatively showed become more prominent; however, we leave a detailed study of their properties such as density profiles to future work.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Warmth elevating the depths: shallower voids with warm dark matter

Yang

Neyrinck

Aragón-Calvo

et al. 2015

Mon. Not. R. Astron. Soc.

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Warm dark matter (WDM) has been proposed as an alternative to cold dark matter (CDM), to resolve issues such as the apparent lack of satellites around the Milky Way. Even if WDM is not the answer to observational issues, it is essential to constrain the nature of the dark matter. The effect of WDM on haloes has been extensively studied, but the small-scale initial smoothing in WDM also affects the present-day cosmic web and voids. It suppresses the cosmic "sub-web" inside voids, and the formation of both void haloes and subvoids. In N -body simulations run with different assumed WDM masses, we identify voids with the zobov algorithm, and cosmic-web components with the origami algorithm. As dark-matter warmth increases (i.e., particle mass decreases), void density minima grow shallower, while void edges change little. Also, the number of subvoids decreases. The density field in voids is particularly insensitive to baryonic physics, so if void density profiles and minima could be measured observationally, they would offer a valuable probe of the nature of dark matter. Furthermore, filaments and walls become cleaner, as the substructures in between have been smoothed out; this leads to a clear, mid-range peak in the density PDF.

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Section: Conclusion and Discussionmentioning

confidence: 99%

Warmth elevating the depths: shallower voids with warm dark matter

Yang

Neyrinck

Aragón-Calvo

et al. 2015

Mon. Not. R. Astron. Soc.

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“…For estimating the cross-correlation function, we randomly distributed the Lyαabsorbers within±600 km s −1 of the galaxy systemic velocity. Therefore, it is not advisable to compare this analysis with blind galaxy-absorber cross-correlation functions, such as those published by Lanzetta et al (1998) Tejos et al (2012), and others. We also considered each component of the Lyαabsorption features as an individual absorber.…”

Section: Kinematicsmentioning

confidence: 99%

The Properties of the Circumgalactic Medium in Red and Blue Galaxies: Results From the Cos-Gass+cos-Halos Surveys

Borthakur

Heckman

Tumlinson

et al. 2016

ApJ

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We use the combined data from the COS-GASS and COS-Halos surveys to characterize the Circum-Galactic Medium (CGM) surrounding typical low-redshift galaxies in the mass range  *~-M M 10 9.5 11.5, and over a range of impact parameters extending to just beyond the halo virial radius (R vir ). We find the radial scale length of the distributions of the equivalent widths of the Lyαand Si III absorbers to be ∼1 and ∼0.4R vir , respectively. The radial distribution of equivalent widths is relatively uniform for the blue galaxies, but highly patchy (i.e., it has a low covering fraction) for the red galaxies. We also find that the Lyαand Si III equivalent widths show significant positive correlations with the specific star formation rate (sSFR) of the galaxy. We find a surprising lack of correlations between the halo mass (virial velocity) and either the velocity dispersions or velocity offsets of the Lyαlines. The ratio of the velocity offset to the velocity dispersion for the Lyαabsorbers has a mean value of ∼4, suggesting that a given line of sight is intersecting a dynamically coherent structure in the CGM, rather than a sea of orbiting clouds. The kinematic properties of the CGM are similar in the blue and red galaxies, although we find that a significantly larger fraction of the blue galaxies have large Lyαvelocity offsets (>200 km s −1 ). We show that-if the CGM clouds represent future fuel for star formation-our new results could imply a large drop in the sSFR across the galaxy mass-range we probe.

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“…This phenomenon suggests a deeper, underlying causal relationship between group galaxies and the larger dark matter halos in which they reside. While the question naturally arises whether environmental effects manifest in the CGM, research on the matter (Tejos et al 2012;Yoon & Putman 2013;Johnson et al 2014Johnson et al , 2015Wakker et al 2015;Finn et al 2016) is in its infancy.…”

Section: Introductionmentioning

confidence: 99%

A DEEP SEARCH FOR FAINT GALAXIES ASSOCIATED WITH VERY LOW REDSHIFT C iv ABSORBERS. III. THE MASS- AND ENVIRONMENT-DEPENDENT CIRCUMGALACTIC MEDIUM

Burchett

Tripp

Bordoloi

et al. 2016

ApJ

107

170

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Using Hubble Space Telescope Cosmic Origins Spectrograph observations of 89 QSO sightlines through the Sloan Digital Sky Survey footprint, we study the relationships between C iv absorption systems and the properties of nearby galaxies as well as large-scale environment. To maintain sensitivity to very faint galaxies, we restrict our sample to 0.0015 < z < 0.015, which defines a complete galaxy survey to L 0.01 L * or stellar mass M * 10 8 M . We report two principal findings. First, for galaxies with impact parameter ρ < 1 r vir , C iv detection strongly depends on the luminosity/stellar mass of the nearby galaxy. C iv is preferentially associated with galaxies with M * > 10 9.5 M ; lower mass galaxies rarely exhibit significant C iv absorption (covering fraction f C = 9 +12 −6 % for 11 galaxies with M * < 10 9.5 M ). Second, C iv detection within the M * > 10 9.5 M population depends on environment. Using a fixed-aperture environmental density metric for galaxies with ρ < 160 kpc at z < 0.055, we find that 57 +12 −13 % (8/14) of galaxies in low-density regions (regions with fewer than seven L > 0.15 L * galaxies within 1.5 Mpc) have affiliated C iv absorption; however, none (0/7) of the galaxies in denser regions show C iv. Similarly, the C iv detection rate is lower for galaxies residing in groups with dark-matter halo masses of M halo > 10 12.5 M . In contrast to C iv, H i is pervasive in the CGM without regard to mass or environment. These results indicate that C iv absorbers with log N (C iv) 13.5 cm −2 trace the halos of M * > 10 9.5 M galaxies but also reflect larger scale environmental conditions.

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Large-scale structure in absorption: gas within and around galaxy voids

Cited by 33 publications

References 97 publications

Warmth elevating the depths: shallower voids with warm dark matter

Warmth elevating the depths: shallower voids with warm dark matter

The Properties of the Circumgalactic Medium in Red and Blue Galaxies: Results From the Cos-Gass+cos-Halos Surveys

A DEEP SEARCH FOR FAINT GALAXIES ASSOCIATED WITH VERY LOW REDSHIFT C iv ABSORBERS. III. THE MASS- AND ENVIRONMENT-DEPENDENT CIRCUMGALACTIC MEDIUM

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