An ISO–SWS survey of molecular hydrogen in starburst  and Seyfert
galaxies

Rigopoulou, D.; Kunze, D.; Lutz, D.; Genzel, R.; Moorwood, A. F. M.

doi:10.1051/0004-6361:20020607

Cited by 130 publications

(203 citation statements)

References 38 publications

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“…Several transitions have been studied with ISO (Rigopoulou et al 2002) and Spitzer (Beirão et al 2008). Both studies agree that the S(1) to S(2) line ratio suggests T ∼ 500 K (assuming an ortho-to-para ratio of 3), in excellent agreement with our temperature.…”

Section: Resultssupporting

confidence: 85%

Probing the molecular interstellar medium of M82 withHerschel-SPIRE spectroscopy

Panuzzo¹,

Rangwala

Rykala

et al. 2010

A&A

118

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We present the observations of the starburst galaxy M82 taken with the Herschel SPIRE Fourier-transform spectrometer. The spectrum (194-671 μm) shows a prominent CO rotational ladder from J = 4-3 to 13-12 emitted by the central region of M82. The fundamental properties of the gas are well constrained by the high J lines observed for the first time. Radiative transfer modeling of these high-S/N 12 CO and 13 CO lines strongly indicates a very warm molecular gas component at ∼500 K and pressure of ∼3 × 10 6 K cm −3 , in good agreement with the H 2 rotational lines measurements from Spitzer and ISO. We suggest that this warm gas is heated by dissipation of turbulence in the interstellar medium (ISM) rather than X-rays or UV flux from the straburst. This paper illustrates the promise of the SPIRE FTS for the study of the ISM of nearby galaxies.

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Section: Resultssupporting

confidence: 85%

Probing the molecular interstellar medium of M82 withHerschel-SPIRE spectroscopy

Panuzzo¹,

Rangwala

Rykala

et al. 2010

A&A

118

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“…rotational H 2 transitions as well as the intermediate-J CO transitions became accessible for a large number of local galaxies (e.g., Rigopoulou et al 2002;Roussel et al 2007;van der Werf et al 2010;Pereira-Santaella et al 2013). Therefore, now for the first time, it is possible to obtain a complete snapshot of molecular gas emission and study its physical properties (temperature, density, column density, etc.)…”

Section: ) Thementioning

confidence: 99%

“…Similarly, when the mid-IR rotational H 2 transitions are analyzed, models with two components are used (e.g., Rigopoulou et al 2002;Roussel et al 2007). In these studies, the derived T kin are always higher than ∼100 K since at lower temperatures the rotational H 2 emission is negligible.…”

Section: Radiative Transfer Modelsmentioning

confidence: 99%

Warm molecular gas temperature distribution in six local infrared bright Seyfert galaxies

Pereira-Santaella

Spinoglio

Werf

et al. 2014

A&A

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We simultaneously analyze the spectral line energy distributions (SLEDs) of CO and H 2 of six local luminous infrared (IR) Seyfert galaxies. For the CO SLEDs, we used new Herschel/SPIRE FTS data (from J = 4-3 to J = 13-12) and ground-based observations for the lower-J CO transitions. The H 2 SLEDs were constructed using archival mid-IR Spitzer/IRS and near-IR VLT/SINFONI data for the rotational and ro-vibrational H 2 transitions, respectively. In total, the SLEDs contain 26 transitions with upper level energies between 5 and 15 000 K. A single, constant density, model (n H 2 ∼ 10 4.5−6 cm −3 ) with a broken power-law temperature distribution reproduces well both the CO and H 2 SLEDs. The power-law indices are β 1 ∼ 1-3 for warm molecular gas (20 K< T < 100 K) and β 2 ∼ 4-5 for hot molecular gas (T > 100 K). We show that the steeper temperature distribution (higher β) for hot molecular gas can be explained by shocks and photodissociation region (PDR) models; however, the exact β values are not reproduced by PDR or shock models alone and a combination of both is needed. We find that the three major mergers among our targets have shallower temperature distributions for warm molecular gas than the other three spiral galaxies. This can be explained by a higher relative contribution of shock excitation, with respect to PDR excitation, for the warm molecular gas in these mergers. For only one of the mergers, IRASF 05189-2524, the shallower H 2 temperature distribution differs from that of the spiral galaxies. The presence of a bright active galactic nucleus in this source might explain the warmer molecular gas observed.

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“…The arrows outline these inflows and outflows, and the gas cooling and heating. H 2 is a key actor in all stages molecular hydrogen emission lines but with relatively weak total IR emission, [2,6,15,17]. In these galaxies, the S(5) line at 6.9 μm is observed to be comparably bright to the S(1) and S(3) lines.…”

Section: How Is the Luminous Universe Taking Shape?mentioning

confidence: 99%

The molecular hydrogen explorer H2EX

et al. 2008

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The Molecular Hydrogen Explorer, H2EX, was proposed in response to the ESA 2015 -2025 Cosmic Vision Call as a medium class space mission with NASA and CSA participations. The mission, conceived to understand the formation of galaxies, stars and planets from molecular hydrogen, is designed to observe the first rotational lines of the H 2 molecule (28.2, 17.0, 12.3 and 9.7 μm) over a wide field, and at high spectral resolution. H2EX can provide an inventory of warm (≥ 100 K) molecular gas in a broad variety of objects, including nearby young star clusters, galactic molecular clouds, active galactic nuclei, local and distant galaxies. The rich array of molecular, atomic and ionic lines, as well as solid state features available in the 8 to 29 μm spectral range brings additional science dimensions to H2EX. We present the optical and mechanical design of the H2EX payload based on an innovative Imaging Fourier Transform Spectrometer fed by a 1.2 m telescope. The 20'×20' field of view is imaged on two 1024×1024 Si:As detectors. The maximum resolution of 0.032 cm −1 (full width at half maximum) means a velocity resolution of 10 km s −1 for the 0 -0 S(3) line at 9.7 μm. This instrument offers the large field of view necessary to survey extended emission in the Galaxy and local Universe galaxies as well as to perform unbiased extragalactic and circumstellar disks surveys. The high spectral resolution makes H2EX uniquely suited to study the dynamics of H 2 in all these environments. The mission plan is made of seven wide-field spectro-imaging legacy programs, from the cosmic web to galactic young star clusters, within a nominal two years mission. The payload has been designed to re-use the Planck platform and passive cooling design.

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An ISO–SWS survey of molecular hydrogen in starburst and Seyfert galaxies

Cited by 130 publications

References 38 publications

Probing the molecular interstellar medium of M82 withHerschel-SPIRE spectroscopy

Probing the molecular interstellar medium of M82 withHerschel-SPIRE spectroscopy

Warm molecular gas temperature distribution in six local infrared bright Seyfert galaxies

The molecular hydrogen explorer H2EX

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