Absorption‐Line Probes of Gas and Dust in Galactic Superwinds

Heckman, Timothy M.; Lehnert, M. D.; Strickland, David; Armus, L.

doi:10.1086/313421

Cited by 636 publications

(1,017 citation statements)

References 132 publications

(257 reference statements)

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“…These estimates range between η ∼ 0.3-30 in this galactic mass range for z ∼ 0.1 (Rupke & Veilleux 2013;Heckman et al 2000;Bouché et al 2012;Bolatto et al 2013). At high redshifts, the estimates appear to be similar to values at present epoch Newman et al 2012).…”

Section: Introductionsupporting

confidence: 64%

Long way to go: how outflows from large galaxies propagate through the hot halo gas

Sarkar

Nath

Sharma

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Using hydrodynamic simulations, we study the mass loss due to supernova-driven outflows from Milky Way type disk galaxies, paying particular attention to the effect of the extended hot halo gas. We find that the total mass loss at inner radii scales roughly linearly with total mass of stars formed, and that the mass loading factor at the virial radius can be several times its value at inner radii because of the swept up hot halo gas. The temperature distribution of the outflowing material in the inner region (∼10 kpc) is bimodal in nature, peaking at 10 5 K and 10 6.5 K, responsible for optical and X-ray emission, respectively. The contribution of cold/warm gas with temperature 10 5.5 K to the outflow rate within 10 kpc is ≈ 0.3-0.5. The warm mass loading factor, η 3e5 (T 3 × 10 5 K) is related to the mass loading factor at the virial radius (η v ) as η v ≈ 25 η 3e5 SFR/M ⊙ yr −1 −0.15 for a baryon fraction of 0.1 and a starburst period of 50 Myr. We also discuss the effect of multiple bursts that are separated by both short and long periods. The outflow speed at the virial radius is close to the sound speed in the hot halo, 200 km s −1 . We identify two 'sequences' of outflowing cold gas at small scales: a fast (≈ 500 km s −1 ) sequence, driven by the unshocked free-wind; and a slow sequence (≈ ±100 km s −1 ) at the conical interface of the superwind and the hot halo.

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Section: Introductionsupporting

confidence: 64%

Long way to go: how outflows from large galaxies propagate through the hot halo gas

Sarkar

Nath

Sharma

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…They found the equivalent widths of the purely stellar features to be correlated as EW NaD ∼ 0.5 EW Mg b , with a possible intrinsic scatter of > ∼ 25%. Heckman et al (2000) combined the data from Heckman et al (1980) with stellar library data from Jacoby et al (1984), and estimated EW NaD ∼ 0.75 EW Mg b , which agrees with their own K giant spectra to within 0.10 dex. Schwartz & Martin (2004) also make a fit to the data by Jacoby et al (1984) to find EW NaD = 0.40±0.05 EW Mg b .…”

Section: Possible Stellar Contamination Of Na Dsupporting

confidence: 56%

“…We note also that other Na D absorption spectra in the literature often show considerably stronger lines (e.g. Heckman et al 2000;Martin 2005). Our conclusion is that the Na D covering fraction is indeed low in these regions.…”

Section: Interpretation Of the Covering Fractions Optical Depths Andsupporting

confidence: 50%

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Neutral gas in Lyman-alpha emitting galaxies Haro 11 and ESO 338-IG04 measured through sodium absorption

Sandberg

Östlin

Hayes

et al. 2013

A&A

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Context. The Lyman alpha emission line of neutral hydrogen is an important tool for finding galaxies at high redshift, thus for probing the structure of the early universe. However, the resonance nature of the line and its sensitivity to dust and neutral gas is still not fully understood.Aims. We present measurements of the velocity, covering fraction and optical depth of neutral gas in front of two well-known, local blue compact galaxies that show Lyman alpha in emission: ESO 338-IG 04 and Haro 11. We thus observationally test the hypothesis that Lyman alpha can escape through neutral gas by being Doppler shifted out of resonance. Methods. We present integral field spectroscopy, obtained with the GIRAFFE/Argus spectrograph at VLT/FLAMES in Paranal, Chile. The excellent wavelength resolution allowed us to accurately measure the velocity of the ionized and neutral gas through the Hα emission and Na D absorption, which trace the ionized medium and cold interstellar gas, respectively. We also present independent measurements from the VLT/X-shooter spectrograph that confirm our results. Results. For ESO 338-IG04 we measure no significant shift of neutral gas: the best fit velocity offset is −15 ± 16 km s −1 . For Haro 11, we see an outflow from knot B at 44 ± 13 km s −1 , and infalling gas towards knot C with 32 ± 12 km s −1 . Based on the relative strength of the Na D absorption lines, we estimate low covering fractions of neutral gas (down to 10%) in all three cases. Conclusions. The Na D absorption most likely occurs in dense clumps with higher column densities than the medium in which the bulk of the Ly α scattering takes place. Still, we find no strong correlation between outflowing neutral gas and strong Ly α emission. The Ly α photons from these two galaxies are therefore likely to be escaping due to a low column density and/or covering fraction.

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“…The merger triggers a powerful nuclear starburst (e.g. Armus, Heckman, & Miley 1987;Sanders et al 1988), which generates strong starburst-driven winds, (Rupke, Veilleux, & Sanders 2005;Veilleux, Cecil, & Bland-Hawthorn 2005;Heckman et al 2000). These winds will eventually blow away the enshrouding dust and lay bare the quasar core, depleting the dust and gas to form an elliptical galaxy (Genzel et al 2001;Veilleux, Kim, & Sanders 2002;Tacconi et al 2002;Dasyra et al 2006a,b).…”

Section: Introductionmentioning

confidence: 99%

J1649+2635: a grand-design spiral with a large double-lobed radio source

Mao

Owen

Duffin

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We report the discovery of a grand-design spiral galaxy associated with a double-lobed radio source. J1649+2635 (z = 0.0545) is a red spiral galaxy with a prominent bulge that it is associated with a L 1.4 GHz ∼10 24 W Hz −1 double-lobed radio source that spans almost 100 kpc. J1649+2635 has a black hole mass of M BH ∼ 3-7 × 10 8 M ⊙ and SFR ∼ 0.26 -2.6 M ⊙ year −1 . The galaxy hosts a ∼96 kpc diffuse optical halo, which is unprecedented for spiral galaxies. We find that J1649+2635 resides in an overdense environment with a mass of M dyn = 7.7 +7.9 −4.3 × 10 13 M ⊙ , likely a galaxy group below the detection threshold of the ROSAT All-Sky Survey. We suggest one possible scenario for the association of double-lobed radio emission from J1649+2635 is that the source may be similar to a Seyfert galaxy, located in a denser-than-normal environment. The study of spiral galaxies that host large-scale radio emission is important because although rare in the local Universe, these sources may be more common at high-redshifts.

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Absorption‐Line Probes of Gas and Dust in Galactic Superwinds

Cited by 636 publications

References 132 publications

Long way to go: how outflows from large galaxies propagate through the hot halo gas

Long way to go: how outflows from large galaxies propagate through the hot halo gas

Neutral gas in Lyman-alpha emitting galaxies Haro 11 and ESO 338-IG04 measured through sodium absorption

J1649+2635: a grand-design spiral with a large double-lobed radio source

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