A<i>Chandra</i>X‐Ray Investigation of the Violent Interstellar Medium: From Dwarf Starbursts to Ultraluminous Infrared Galaxies

Grimes, John; Heckman, Timothy M.; Strickland, David; Ptak, Andrew

doi:10.1086/430692

Cited by 103 publications

(208 citation statements)

References 53 publications

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“…However, these values are relatively high when compared to the study by Strickland et al (2004), who obtained kT = 0.11 keV and kT = 0.37 keV for a two-temperature model fitted simultaneously to eight starbursts whose X-ray point-sources had been removed. Also, Grimes et al (2005) only found two sources with kT > 0.5 keV among seven dwarf starbursts. The kT value we propose for Haro 2 agrees better with the values found by Grimes et al (2005) for their sample of ULIRGs.…”

Section: ) Obtaining Best Fits When O and Mg Abundances Were Z(omentioning

confidence: 91%

“…Also, Grimes et al (2005) only found two sources with kT > 0.5 keV among seven dwarf starbursts. The kT value we propose for Haro 2 agrees better with the values found by Grimes et al (2005) for their sample of ULIRGs. As previously said, hard emission in Haro 2 is dominated by the point-like source X1.…”

Section: ) Obtaining Best Fits When O and Mg Abundances Were Z(omentioning

confidence: 91%

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Multiwavelength analysis of the Lyman-αemitting galaxy Haro 2: relation between the diffuse Lyman-αand soft X-ray emissions

Otí-Floranes

Mas-Hesse

Jiménez‐Bailón

et al. 2012

A&A

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Context. Lyman-α emission is commonly used as star formation tracer in cosmological studies. Nevertheless, resonant scattering strongly affects the resulting luminosity, leading to variable and unpredictable escape fractions in different objects. Aims. To understand how the Lyα escape fraction depends on the properties of the star-forming regions, we need high spatial resolution multiwavelength studies of nearby Lyα emitters, like Haro 2. Methods. We study the Lyα emission of Haro 2 in connection with the properties of the young stellar population, the characteristics of the interstellar medium, the distribution and intensity of the Balmer emission lines and the properties of the X-ray emission. We have used HST-STIS spectral images along the major and minor axes of Haro 2 to characterize the Lyα emission, as well as FOC UV, WFPC-2 optical and NICMOS near infrared broadband-filter images to analyze the properties of the stellar population. WFPC-2 Hα image and ground-based spectroscopy allow us to study the Balmer emission lines. Finally, Chandra/ACIS X-ray images provide resolved distribution of the X-ray emission at various energy bands. The observational data are analyzed by comparison with the predictions from evolutionary synthesis models to constrain the properties of the star formation episode. Results. The UV, Hα and far infrared luminosities of the Haro 2 nuclear starburst are well reproduced assuming a young stellar population with ages ∼3.5-5.0 Myr, affected by differential intestellar extinctions. A significant fraction of the stars are completely obscured in the UV, being identifiable only indirectly by their contribution to the ionization of the gas and to the far infrared emission. The diffuse soft X-ray emission extending over the whole source is attributed to gas heated by the mechanical energy released by the starburst. A compact hard X-ray emission (likely an UltraLuminous X-ray source) has been identified in a star-forming condensation to the southeast. Both compact and diffuse Lyα emission components are observed along the major and minor axes in STIS spectral images. Lyα is spatially decoupled from Balmer lines emission, Balmer decrement and UV continuum. However, the diffuse Lyα component is spatially correlated with the diffuse soft X-ray emission. Moreover, unlike the compact Lyα emission, diffuse Lyα shows luminosities larger than predicted from Hα, assuming case B recombination and considering the dust extinction as derived from Hα/Hβ. Conclusions. The Lyα emission closely associated to the massive stellar clusters is strongly affected by the properties of the surrounding neutral gas (presence of outflows, dust abundance), leading to even a range of escape fractions at different locations within the same starburst. On the other hand, we propose that the diffuse Lyα emission originates in gas ionized by the hot plasma responsible for the soft X-ray radiation, as suggested by their spatial correlation and by the measured L(Hα)/L 0.4−2.4 keV ratios. Calibration of Lyα as star forma...

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Section: ) Obtaining Best Fits When O and Mg Abundances Were Z(omentioning

confidence: 91%

Section: ) Obtaining Best Fits When O and Mg Abundances Were Z(omentioning

confidence: 91%

Multiwavelength analysis of the Lyman-αemitting galaxy Haro 2: relation between the diffuse Lyman-αand soft X-ray emissions

Otí-Floranes

Mas-Hesse

Jiménez‐Bailón

et al. 2012

A&A

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“…Indeed, the center of NGC 3628 resembles that of NGC 660 also by its complement of compact radio continuum sources (none coinciding with the nucleus) representing active regions in the circumnuclear star-burst contributing about 10% to the total radio continuum emission (Carral et al 1990), and by its H92α radio recombination line emission from high-density HII regions (n HII ≈ 10 4 cm −3 -Anantharamaiah et al 1993;Zhao et al 1997). The central core of NGC 3628 is also bright in X-rays, and the galaxy has an extended halo of soft X-ray emission surrounding a central outflow, apparently a galactic (star-burstdriven) super-wind bubble (Dahlem et al 1996(Dahlem et al , 1998Strickland et al 2004a,b;Grimes et al 2005;Flohic et al 2006). NGC 3628 may (Roberts et al 2001;González-Martín et al 2006) or may not (Dudik et al 2005) contain a low-luminosity AGN.…”

Section: Ngc 3628mentioning

confidence: 99%

CI and CO in nearby galaxy centers

Israel¹

2009

A&A

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Aims. We study the physical properties and mass of molecular gas in the central regions of galaxies with active nuclei. Methods. Maps and measurements of the J = 1-0, J = 2-1, J = 3-2, J = 4-3 12 CO, the J = 1-0, J = 2-1 and J = 3-2 13 CO lines in the central arcminute squared of NGC 278, NGC 660, NGC 3628, NGC 4631, and NGC 4666, as well as 492 GHz [CI] maps in three of these are used to model the molecular gas. Results. All five objects contain bright CO emission in the central regions. Clear central concentrations were found in NGC 660, NGC 3628, and NGC 4666, but not in the weakest CO emitters NGC 278 and NGC 4631. In all cases, the observed lines could be modeled only with at least two distinct gas components. The physical condition of the molecular gas is found to differ from galaxy to galaxy. Relatively tenuous (density 100-1000 cm −3 ) and high kinetic temperature (100-150 K) gas occur in all galaxies, except perhaps NGC 3628, mixed with cooler (10-30 K) and denser (0.3−1.0 × 10 4 cm −3 ) gas. The CO-to-H 2 conversion factor X is typically an order of magnitude less than the "standard" value in the Solar Neighborhood in all galaxy centers. The molecular gas is constrained within radii between 0.6 and 1.5 kpc from the nuclei. Within these radii, H 2 masses are typically 0.6−1.5 × 10 8 M , which corresponds to no more than a few per cent of the dynamical mass in the same region.

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“…Outflows are commonly observed in local U/LIRGs Rupke & Veilleux 2005;Rupke et al 2005a,b,c;Martin 2006;Sturm et al 2011;Rupke & Veilleux 2013;Veilleux et al 2013;Teng et al 2013;Spoon et al 2013;Rodríguez Zaurín et al 2013;Arribas et al 2014;Cicone et al 2014), and are likely a common cause of shocks. Several studies of shocks in nearby galaxies have linked them to superwinds produced by stellar feedback (Heckman et al 1990;Grimes et al 2005;Rich et al 2011;Hopkins et al 2012;Hong et al 2013) and AGN-driven outflows (Mazzarella et al 2012). Although these systems are relatively rare in the local universe, Le Floc'h et al (2005) have shown that high infrared luminosities may have been the norm at redshifts beyond 0.7.…”

Section: Introductionmentioning

confidence: 99%

Shocked gas in IRAS F17207-0014: ISM collisions and outflows

Medling

Vivian

Kewley

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We combine optical and near-infrared AO-assisted integral field observations of the merging ULIRG IRAS F17207-0014 from the Wide-Field Spectrograph (WiFeS) and Keck/OSIRIS. The optical emission line ratios [N II]/Hα, [S II]/Hα, and [O I]/Hα reveal a mixing sequence of shocks present throughout the galaxy, with the strongest contributions coming from large radii (up to 100% at ∼5 kpc in some directions), suggesting galactic-scale winds. The nearinfrared observations, which have approximately 30 times higher spatial resolution, show that two sorts of shocks are present in the vicinity of the merging nuclei: low-level shocks distributed throughout our field-of-view evidenced by an H 2 /Brγ line ratio of ∼0.6-4, and strong collimated shocks with a high H 2 /Brγ line ratio of ∼4-8, extending south from the two nuclear disks approximately 400 pc (∼0. ′′ 5). Our data suggest that the diffuse shocks are caused by the collision of the interstellar media associated with the two progenitor galaxies and the strong shocks trace the base of a collimated outflow coming from the nucleus of one of the two disks.

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AChandraX‐Ray Investigation of the Violent Interstellar Medium: From Dwarf Starbursts to Ultraluminous Infrared Galaxies

Cited by 103 publications

References 53 publications

Multiwavelength analysis of the Lyman-αemitting galaxy Haro 2: relation between the diffuse Lyman-αand soft X-ray emissions

Multiwavelength analysis of the Lyman-αemitting galaxy Haro 2: relation between the diffuse Lyman-αand soft X-ray emissions

CI and CO in nearby galaxy centers

Shocked gas in IRAS F17207-0014: ISM collisions and outflows

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