Suppression of star formation in the galaxy NGC 253 by a starburst-driven molecular wind

Bolatto, Alberto D.; Warren, Steven R.; Leroy, Adam K.; Walter, Fabian; Veilleux, Sylvain; Ostriker, Eve C.; Ott, J.; Zwaan, M. A.; Fisher, David B.; Weiß, A.; Rosolowsky, Erik; Hodge, J. A.

doi:10.1038/nature12351

Cited by 278 publications

(372 citation statements)

References 30 publications

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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: 48%

“…These values show the same behaviour as seen previously in η20 only with a shallower dependence on L (η obs ∝ L −0.15 ). However, the estimation of the mass loading factor from observations is either for the cold molecular gas (Bolatto et al 2013) or the ionised (Arribas et al 2014) or the hot gas (Stickland & Heckman 2007), and not for all the phases taken together. Therefore, to determine the mass loading factors for different phases and find the correlation between them, it is important to study the temperature distribution of η obs .…”

Section: Comparison With Observed Mass Loading Factormentioning

confidence: 99%

“…The mass loading factor in observations is defined as η = M ×vr r×SFR , where, M is the total mass of outflowing gas (observed as molecular or ionised gas), r is the typical scale of the outflowing region and vr is an estimate of the outflowing gas velocity (Arribas et al 2014;Bolatto et al 2013) or the sound speed (Stickland & Heckman 2007). In order to compare with the observed values of mass loading factor, we define η obs , the mass loading factor within a outflowing region of radius r d at any time t as where, r d is taken to be 10 kpc, the radius within which most of the observations are limited.…”

Section: Comparison With Observed Mass Loading Factormentioning

confidence: 99%

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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: 48%

Section: Comparison With Observed Mass Loading Factormentioning

confidence: 99%

Section: Comparison With Observed Mass Loading Factormentioning

confidence: 99%

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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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“…Mechanical heating can also be introduced into the ISM through supernova remnants (Loenen et al 2008) or strong jets and we test its efficiency at heating molecular gas using the mPDR and mCDR models. Strong molecular outflows have been observed by Bolatto et al (2013), and they estimate an outflow rate of 9 M yr −1 , implying the outflows are a strong source of turbulence in the galactic nucleus.…”

Section: Application To Ngc 253mentioning

confidence: 99%

Radiative and mechanical feedback into the molecular gas of NGC 253

Rosenberg

Kazandjian

Werf

et al. 2014

A&A

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Starburst galaxies are galaxies or regions of galaxies undergoing intense periods of star formation. Understanding the heating and cooling mechanisms in these galaxies can give us insight to the driving mechanisms that fuel the starburst. Molecular emission lines play a crucial role in the cooling of the excited gas. With Herschel Spectral and Photometric Imaging Receiver we have been able to observe the rich molecular spectrum towards the central region of NGC 253. Carbon monoxide (CO, J = 4−3 to 13−12) is the brightest molecule in the Herschel wavelength range and together with ground-based low-J observations, the line fluxes trace the excitation of CO. By studying the CO excitation ladder and comparing the intensities to models, we investigate whether the gas is excited by UV radiation, X-rays, cosmic rays, or turbulent heating. Comparing the 12 CO and 13 CO observations to large velocity gradient models and photon-dominated region (PDR) models we find three main interstellar medium (ISM) phases. We estimate the density, temperature, and masses of these ISM phases. By adding 13 CO, HCN, and HNC line intensities, we are able to constrain these degeneracies and determine the heating sources. The first ISM phase responsible for the low-J CO lines is excited by PDRs, but the second and third phases, responsible for the mid to high-J CO transitions, require an additional heating source. We find three possible combinations of models that can reproduce our observed molecular emission. Although we cannot determine which of these is preferable, we can conclude that mechanical heating is necessary to reproduce the observed molecular emission and cosmic ray heating is a negligible heating source. We then estimate the mass of each ISM phase; 6 × 10 7 M for phase 1 (low-J CO lines), 3 × 10 7 M for phase 2 (mid-J CO lines), and 9 × 10 6 M for phase 3 (high-J CO lines) for a total system mass of 1 × 10 8 M .

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“…4.1) suggests that the outflow has a significant component that is oriented perpendicular to the rotating disk. This geometry is typically found in star-forming-driven molecular outflows, like the ones discovered in the starbursts M 82 and NGC 253 (García-Burillo et al 2001;Walter et al 2002;Bolatto et al 2013b;Salas et al 2014). However, we cannot exclude that an AGN can also contribute to drive the outflow (see discussion in Sect.…”

Section: A Non-coplanar Outflow Solutionmentioning

confidence: 99%

High-resolution imaging of the molecular outflows in two mergers: IRAS 17208-0014 and NGC 1614

García‐Burillo

Combes

Usero

et al. 2015

A&A

107

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Context. Galaxy evolution scenarios predict that the feedback of star formation and nuclear activity (AGN) can drive the transformation of gas-rich spiral mergers into (ultra) luminous infrared galaxies and, eventually, lead to the build-up of QSO/elliptical hosts. Aims. We study the role that star formation and AGN feedback have in launching and maintaining the molecular outflows in two starburst-dominated advanced mergers, NGC 1614 (D L = 66 Mpc) and IRAS 17208-0014 (D L = 181 Mpc), by analyzing the distribution and kinematics of their molecular gas reservoirs. Both galaxies present evidence of outflows in other phases of their ISM. Methods. We used the Plateau de Bure interferometer (PdBI) to image the CO(1-0) and CO(2-1) line emissions in NGC 1614 and IRAS 17208-0014, respectively, with high spatial resolution (0. 5-1. 2). The velocity fields of the gas were analyzed and modeled to find the evidence of molecular outflows in these sources and characterize the mass, momentum, and energy of these components. Results. While most (≥95%) of the CO emission stems from spatially resolved (∼2−3 kpc-diameter) rotating disks, we also detect in both mergers the emission from high-velocity line wings that extend up to ±500-700 km s −1 , well beyond the estimated virial range associated with rotation and turbulence. The kinematic major axis of the line-wing emission is tilted by ∼90 • in NGC 1614 and by ∼180 • in IRAS 17208-0014 relative to the major axes of their respective rotating disks. These results can be explained by the existence of non-coplanar molecular outflows in both systems: the outflow axis is nearly perpendicular to the rotating disk in NGC 1614, but it is tilted relative to the angular momentum axis of the rotating disk in IRAS 17208-0014. Conclusions. In stark contrast to NGC 1614, where star formation alone can drive its molecular outflow, the mass, energy, and momentum budget requirements of the molecular outflow in IRAS 17208-0014 can be best accounted for by the existence of a so far undetected (hidden) AGN of L AGN ∼ 7 × 10 11 L . The geometry of the molecular outflow in IRAS 17208-0014 suggests that the outflow is launched by a non-coplanar disk that may be associated with a buried AGN in the western nucleus.

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Suppression of star formation in the galaxy NGC 253 by a starburst-driven molecular wind

Cited by 278 publications

References 30 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

Radiative and mechanical feedback into the molecular gas of NGC 253

High-resolution imaging of the molecular outflows in two mergers: IRAS 17208-0014 and NGC 1614

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