EXTENDED HCN AND HCO<sup>+</sup>EMISSION IN THE STARBURST GALAXY M82

Salas, P.; Galaz, Gaspar; Salter, D. M.; Herrera-Camus, R.; Bolatto, Alberto D.; Kepley, Amanda A.

doi:10.1088/0004-637x/797/2/134

Cited by 21 publications

(21 citation statements)

References 55 publications

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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: 62%

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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Section: A Non-coplanar Outflow Solutionmentioning

confidence: 62%

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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“…(1) Nishimura et al (2016); (2) Watanabe et al (2014); (3) Aladro et al (2015); (4) Salas et al (2014); (5) Meier et al (2015); (6) Meier & Turner (2012); (7) Nishimura et al (2016). (8) This work.…”

Section: Dense Gas Tracersmentioning

confidence: 99%

The anatomy of the Orion B giant molecular cloud: A local template for studies of nearby galaxies

Pety

Guzmán

Orkisz

et al. 2017

A&A

197

319

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Context. Molecular lines and line ratios are commonly used to infer properties of extra-galactic star forming regions. The new generation of millimeter receivers almost turns every observation into a line survey. Full exploitation of this technical advancement in extra-galactic study requires detailed bench-marking of available line diagnostics. Aims. We aim to develop the Orion B giant molecular cloud (GMC) as a local template for interpreting extra-galactic molecular line observations. Methods. We use the wide-band receiver at the IRAM-30 m to spatially and spectrally resolve the Orion B GMC. The observations cover almost 1 square degree at 26 resolution with a bandwidth of 32 GHz from 84 to 116 GHz in only two tunings. Results. We introduce the molecular anatomy of the Orion B GMC, including relationships between line intensities and gas column density or far-UV radiation fields, and correlations between selected line and line ratios. We also obtain a dust-traced gas mass that is less than approximately one third the CO-traced mass, using the standard X CO conversion factor. The presence of over-luminous CO can be traced back to the dependence of the CO intensity on UV illumination. As a matter of fact, while most lines show some dependence on the UV radiation field, CN and C 2 H are the most sensitive. Moreover, dense cloud cores are almost exclusively traced by N 2 H + . Other traditional high-density tracers, such as HCN(1−0), are also easily detected in extended translucent regions at a typical density of ∼500 H 2 cm −3 . In general, we find no straightforward relationship between line critical density and the fraction of the line luminosity coming from dense gas regions. Conclusions. Our initial findings demonstrate that the relationships between line (ratio) intensities and environment in GMCs are more complicated than often assumed. Sensitivity (i.e., the molecular column density), excitation, and, above all, chemistry contribute to the observed line intensity distributions, and they must be considered together when developing the next generation of extra-galactic molecular line diagnostics of mass, density, temperature, and radiation field.

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“…Its proximity (3.89 Mpc; Sakai & Madore 1999) allows us to investigate in detail the starburst activity and its relationship with the superwind. Many observational studies have been done for the superwind of this galaxy (Bland & Tully 1988;Heckman, Armus & Miley 1990;Brouillet & Schilke 1993;Bregman, Schulman & Tomisaka 1995;Shopbell & Bland-Hawthorn 1998;Kaaret et al 2001;Ohyama et al 2002;Hoopes et al 2005;Engelbracht et al 2006;Tsuru et al 2007;Strickland & Heckman 2009;Leeuw & Robson 2009;Veilleux, Rupke & Swaters 2009;Westmoquette et al 2009;Kaneda et al 2010;Contursi et al 2013;Salak et al 2013;Salas et al 2014;Bierão et al 2015;Leroy et al 2015). The superwind of M82 is well known to be highly dusty.…”

Section: Introductionmentioning

confidence: 99%

Spectropolarimetry of the superwind filaments of the starburst galaxy M 82 II: Kinematics of the dust surrounding the nuclear starburst

Yoshida

Kawabata

Ohyama

et al. 2019

Publications of the Astronomical Society of Japan

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We performed deep spectropolarimetric observations of a prototypical starburst galaxy M82 with the Subaru Telescope in order to study the kinematics of the dust outflow. We obtained optical polarized emission-line spectra up to ∼4 kpc away from the nucleus of the galaxy along three position angles, 138 • , 150 • and 179 • within the conical outflowing wind (superwind). The Hα emission line in the superwind is strongly polarized and the polarization pattern shows dust scattering of central light sources, being consistent with the previous works. The intensity weighted polarization degree of the Hα line reaches ∼30% at maximum. There are at least two light sources at the central region of the galaxy; one of which is located at the nearinfrared nucleus and the other resides at one of the peaks of the 3 mm radio and molecular gas emission. The outer (> 1 kpc) dust is illuminated by the former, whereas the inner dust is scattering the light from the latter. We investigated as well the dust motion from the velocity field of the polarized Hα emission line. The dust is accelerated outward on the northwest side of the nucleus. A simple bi-conical dust outflow model shows that the outflow velocity of the dust reaches > ∼ 300 − 450 km s −1 at ∼ 4 kpc from the nucleus, suggesting that some portion of the dust escapes from the gravitational potential of M82 into the intergalactic space. At some regions on the southeast side, in particular along the position angle of 138 • , the dust has radial velocity slower than the systemic velocity of the galaxy, apparently suggesting inflowing motion toward the nucleus. These components are spatially consistent with a part of the molecular gas stream, which is kinematically independent of the outflow gas, thus the apparent inflow motion of the dust reflects the streaming motion associated with the molecular gas stream.

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EXTENDED HCN AND HCO⁺EMISSION IN THE STARBURST GALAXY M82

Cited by 21 publications

References 55 publications

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

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

The anatomy of the Orion B giant molecular cloud: A local template for studies of nearby galaxies

Spectropolarimetry of the superwind filaments of the starburst galaxy M 82 II: Kinematics of the dust surrounding the nuclear starburst

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EXTENDED HCN AND HCO+EMISSION IN THE STARBURST GALAXY M82

Cited by 21 publications

References 55 publications

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

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

The anatomy of the Orion B giant molecular cloud: A local template for studies of nearby galaxies

Spectropolarimetry of the superwind filaments of the starburst galaxy M 82 II: Kinematics of the dust surrounding the nuclear starburst

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EXTENDED HCN AND HCO⁺EMISSION IN THE STARBURST GALAXY M82