Galactic outflow and diffuse gas properties at z ≥ 1 using different baryonic feedback models

Barai, Paramita; Monaco, Pierluigi; Murante, Giuseppe; Ragagnin, Antonio; Viel, Matteo

doi:10.1093/mnras/stu2340

Cited by 33 publications

(54 citation statements)

References 126 publications

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“…The different lines in Figure 10 represent various theoretical (Okamoto et al 2010;Davé et al 2011;Hopkins et al 2012;Puchwein & Springel 2013;Barai et al 2015;Muratov et al 2015) and empirical models (Peeples & Shankar 2011;Zahid et al 2014). 10 In comparing observations and models, it is important to bear in mind that some are fiducial scaling relations put in the sub-grid physics (e.g., Davé et al 2011;Puchwein & Springel 2013;, while others are from more complex numerical approaches (e.g., Hopkins et al 2012Hopkins et al , 2013Barai et al 2015;Muratov et al 2015) 11 and thus are more directly comparable with observations.…”

Section: Conclusion and Discussionmentioning

confidence: 97%

THE VLT SINFONI Mg ii PROGRAM FOR LINE EMITTERS (SIMPLE). II. BACKGROUND QUASARS PROBING $Z\sim 1$ GALACTIC WINDS

Schroetter

Bouché

Péroux

et al. 2015

ApJ

116

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The physical properties of galactic winds are of paramount importance for our understanding of galaxy formation. Fortunately, they can be constrained using background quasars passing near star-forming galaxies (SFGs). From the 14 quasar-galaxy pairs in our Very Large Telescope (VLT)/SINFONI Mg II Program for Line Emitters sample, we reobserved the 10 brightest galaxies in Hα with the VLT/SINFONI with 0″ . 7 seeing and the corresponding quasar with the VLT/UVES spectrograph. Applying geometrical arguments to these 10 pairs, we find that four are likely probing galactic outflows, three are likely probing extended gaseous disks, and the remaining three are not classifiable because they are viewed face-on. In this paper we present a detailed comparison between the line-ofsight kinematics and the host galaxy emission kinematics for the pairs suitable for wind studies. We find that the kinematic profile shapes (asymmetries) can be well reproduced by a purely geometrical wind model with a constant wind speed, except for one pair (toward J2357−2736) that has the smallest impact parameter b = 6 kpc and requires an accelerated wind flow. Globally, the outflow speeds are ∼100 km s −1 and the mass ejection rates (or Ṁ out ) in the gas traced by the low-ionization species are similar to the star formation rate (SFR), meaning that the mass loading factor, h = Ṁ out SFR, is ≈1.0. The outflow speeds are also smaller than the local escape velocity, which implies that the outflows do not escape the galaxy halo and are likely to fall back into the interstellar medium.

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Section: Conclusion and Discussionmentioning

confidence: 97%

THE VLT SINFONI Mg ii PROGRAM FOR LINE EMITTERS (SIMPLE). II. BACKGROUND QUASARS PROBING $Z\sim 1$ GALACTIC WINDS

Schroetter

Bouché

Péroux

et al. 2015

ApJ

116

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“…We adopt a constant-velocity outflow with vSN = 350 km/s (as was done in e.g. Barai et al 2015;Biffi et al 2016). Stellar evolution and chemical enrichment are computed for the 11 elements (following Tornatore et al 2007).…”

Section: Model)mentioning

confidence: 99%

Quasar outflows at z ≥ 6: the impact on the host galaxies

Barai

Gallerani

Pallottini

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We investigate quasar outflows at z 6 by performing zoom-in cosmological hydrodynamical simulations. By employing the SPH code GADGET-3, we zoom in the 2R 200 region around a 2×1012 M ⊙ halo at z = 6, inside a (500 Mpc) 3 comoving volume. We compare the results of our AGN runs with a control simulation in which only stellar/SN feedback is considered. Seeding 10 5 M ⊙ BHs at the centers of 10 9 M ⊙ halos, we find the following results. BHs accrete gas at the Eddington rate over z = 9 − 6. At z = 6, our most-massive BH has grown to M BH = 4 × 10 9 M ⊙ . Fast (v r > 1000 km/s), powerful (Ṁ out ∼ 2000M ⊙ /yr) outflows of shock-heated low-density gas form at z ∼ 7, and propagate up to hundreds kpc. Star-formation is quenched over z = 8 − 6, and the total SFR (SFR surface density near the galaxy center) is reduced by a factor of 5 (1000). We analyse the relative contribution of multiple physical process: (i) disrupting cosmic filamentary cold gas inflows, (ii) reducing central gas density, (iii) ejecting gas outside the galaxy; and find that AGN feedback has the following effects at z = 6. The inflowing gas mass fraction is reduced by ∼ 12%, the high-density gas fraction is lowered by ∼ 13%, and ∼ 20% of the gas outflows at a speed larger than the escape velocity (500 km/s). We conclude that quasar-host galaxies at z 6 are accreting non-negligible amount of cosmic gas, nevertheless AGN feedback quenches their star formation dominantly by powerful outflows ejecting gas out of the host galaxy halo.

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“…An alternative way to implement the collective effect of SN explosions is the (stochastic) implementation of thermal feedback, where galactic winds develop without imposing any input outflow velocity or mass loading factor such as in the EAGLE simulations (e.g., Schaye et al 2015), the FIRE simulations (Hopkins et al 2014;Muratov et al 2015), and the multi-phase scheme of Barai et al (2015).…”

Section: Cmentioning

confidence: 99%

Muse Gas Flow and Wind (Megaflow). I. First Muse Results on Background Quasars*

Schroetter

Bouché

Wendt

et al. 2016

ApJ

104

122

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The physical properties of galactic winds are one of the keys to understand galaxy formation and evolution. These properties can be constrained thanks to background quasar lines of sight (LOS) passing near star-forming galaxies (SFGs). We present the first results of the MusE GAs FLOw and Wind survey obtained from two quasar fields, which have eight Mg II absorbers of which three have rest equivalent width greater than 0.8 Å. With the new Multi Unit Spectroscopic Explorer (MUSE) spectrograph on the Very Large Telescope (VLT), we detect six (75%) Mg II host galaxy candidates within a radius of 30″ from the quasar LOS. Out of these six galaxy-quasar pairs, from geometrical argument, one is likely probing galactic outflows, where two are classified as "ambiguous," two are likely probing extended gaseous disks and one pair seems to be a merger. We focus on the wind-pair and constrain the outflow using a high-resolution quasar spectra from the Ultraviolet and Visual Echelle Spectrograph. Assuming the metal absorption to be due to ga;s flowing out of the detected galaxy through a cone along the minor axis, we find outflow velocities in the order of ≈150 -km s 1 (i.e., smaller than the escape velocity) with a loading factor, h = M SFR ouṫ , of ≈0.7. We see evidence for an open conical flow, with a low-density inner core. In the future, MUSE will provide us with about 80 multiple galaxy−quasar pairs in two dozen fields.

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Galactic outflow and diffuse gas properties at z ≥ 1 using different baryonic feedback models

Cited by 33 publications

References 126 publications

THE VLT SINFONI Mg ii PROGRAM FOR LINE EMITTERS (SIMPLE). II. BACKGROUND QUASARS PROBING $Z\sim 1$ GALACTIC WINDS

THE VLT SINFONI Mg ii PROGRAM FOR LINE EMITTERS (SIMPLE). II. BACKGROUND QUASARS PROBING $Z\sim 1$ GALACTIC WINDS

Quasar outflows at z ≥ 6: the impact on the host galaxies

Muse Gas Flow and Wind (Megaflow). I. First Muse Results on Background Quasars*

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