Supernova-driven outflows in NGC 7552: a comparison of H α and UV tracers

Wood, Corey M.; Tremonti, Christy; Calzetti, Daniela; Leitherer, Claus; Chisholm, John; Gallagher, John S.

doi:10.1093/mnras/stv1471

Cited by 31 publications

(39 citation statements)

References 75 publications

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“…Not accounting for these nearby can have a large effect on the fitted line profiles and measured velocities. We simultaneously fit the nearby S II, S III and O I lines, where the S column densities are tied to the Si II column density by the Milky Way gas phase abundance ratio (Jenkins 2009 (Wood et al 2015), and we simultaneously fit the Si III 1206 line and the Si IV 1400 doublet, similar to the O I line. While the exact wavelength coverage depends on the setup, every spectra has wavelength coverage of all of the Si II lines fitted (i.e., every spectra covers between 1190 and 1300 Å in the rest-frame).…”

Section: Measuring Si II Velocitiesmentioning

confidence: 99%

Scaling Relations Between Warm Galactic Outflows and Their Host Galaxies

Chisholm¹,

Tremonti²,

Leitherer

et al. 2015

ApJ

Self Cite

163

211

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We report on a sample of 48 nearby, star-forming galaxies observed with the Cosmic Origin Spectrograph on the Hubble Space Telescope. We measure the kinematics of warm gas in galactic outflows using a combination of four Si II absorption lines. We use multi-wavelength ancillary data to estimate stellar masses (M * ), star formation rates (SFR), circular velocities (v circ ), and morphologies. The galaxies cover four orders of magnitude in M * and SFR, and sample a wide range of morphologies from starbursting mergers to normal star-forming galaxies. We derive 3.0-3.5σ relations between outflow velocity and SFR, M * , and v circ . The outflow velocities scale as SFR with the range depending on whether we use a maximum or a central velocity to quantify the outflow velocity. After accounting for their increased SFR, mergers drive 32% faster outflows than nonmerging galaxies, with all of the highest velocity outflows arising from mergers. Low-mass galaxies (log (M * / M e ) < 10.5) lose some low-ionization gas through galactic outflows, while more massive galaxies retain all of their low-ionization gas, unless they undergo a merger.

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Section: Measuring Si II Velocitiesmentioning

confidence: 99%

Scaling Relations Between Warm Galactic Outflows and Their Host Galaxies

Chisholm¹,

Tremonti²,

Leitherer

et al. 2015

ApJ

Self Cite

163

211

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show abstract

“…10 Indeed, the gas responsible for the blueshifted absorption lines in galaxies could be 0.1, 1, or 10 kpc away from the host. Some recent studies have made serious attempts at determining the scaling of outflow rates with galaxy properties by setting the absorbing gas at a fixed distance (Chisholm et al 2015;Heckman et al 2015;Wood 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

107

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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“…For a biconical flow, this wind speed represents the flow speed along any radial trajectories, but if the absorption originates from regions close to the disk where the flow is more cylindrical, V out ought to be corrected for the galaxy inclination ( i cos ) and would be −160km s −1 since the galaxy inclination is~ 60 . Following Leitherer et al (2013), Wood et al (2015), and Heckman et al (2015), one can estimate the hydrogen column density using the gas-to-dust ratio and the relationship between N H and reddening (e.g., Bohlin et al 1978 Wood et al (2015), this value represents an upper limit on the column density, as the extinction traces the column density to the star cluster and thus likely includes contributions from gasin both the disk and the wind. Another lower limit comes from the Mg II rest-frame equivalent widthW 3.5 r 2796 Å (Table 3), which implies a column density >2 10 20 -cm 2 from the Ménard & Chelouche (2009) column density-Mg IIequivalent width correlation, i.e., at least about 40% of the column density is in the wind.…”

Section: Windmentioning

confidence: 99%

POSSIBLE SIGNATURES OF A COLD-FLOW DISK FROM MUSE USING A z ∼ 1 GALAXY–QUASAR PAIR TOWARD SDSS J1422−0001*

Bouché

Finley

Schroetter

et al. 2016

ApJ

110

113

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We use a background quasar to detect the presence of circumgalactic gas around a = z 0.91 low-mass star-forming galaxy. Data from the new Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope show that the galaxy has a dust-corrected star formation rate (SFR) of 4.7±2.0M e yr −1 , with no companion down to 0.22. Using a high-resolution spectrum of the background quasar, which is fortuitously aligned with the galaxy major axis (with an azimuth angle α of only 15°), we find, in the gas kinematics traced by low-ionization lines, distinct signatures consistent with those expected for a "cold-flow disk" extending at least 12 kpc (´R 3 1 2 ). We estimate the mass accretion rate M iṅ to be at least two to three times larger than the SFR, using the geometric constraints from the IFU data and the H I column density of log N H I / -cm 2 ; 20.4 obtained from a Hubble Space Telescope/COS near-UV spectrum. From a detailed analysis of the lowionization lines (e.g., Zn II, Cr II, Ti II, Mn II, Si II), the accreting material appears to be enriched to about 0.4  Z (albeit with large uncertainties:= -  Z Z log 0.4 0.4), which is comparable to the galaxy metallicity (12 + log O/H = 8.7 ± 0.2), implying a large recycling fraction from past outflows. Blueshifted Mg II and Fe II absorptions in the galaxy spectrum from the MUSE data reveal the presence of an outflow. The Mg II and Fe II absorption line ratios indicate emission infilling due to scattering processes, but the MUSE data do not show any signs of fluorescent Fe II * emission.

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Supernova-driven outflows in NGC 7552: a comparison of H α and UV tracers

Cited by 31 publications

References 75 publications

Scaling Relations Between Warm Galactic Outflows and Their Host Galaxies

Scaling Relations Between Warm Galactic Outflows and Their Host Galaxies

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

POSSIBLE SIGNATURES OF A COLD-FLOW DISK FROM MUSE USING A z ∼ 1 GALAXY–QUASAR PAIR TOWARD SDSS J1422−0001*

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