Near‐Infrared Integral Field Spectroscopy and Mid‐Infrared Spectroscopy of the Starburst Galaxy M82

Schreiber, N. M. Förster; Genzel, R.; Lutz, D.; Kunze, D.; Sternberg, A.

doi:10.1086/320546

Cited by 127 publications

(41 citation statements)

References 124 publications

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“…A.2 and A.3 the observed spectral energy distributions of our sample sources with the empirical SED of M 82 scaled to fit the measured LW3 flux (thick continuous line). The M 82 SED has been taken partly from Silva et al (1998), partly from the observed ISOCAM-CVF low-resolution spectrum between 5 and 18 µm by Foerster-Schreiber et al (2001), in order to get a proper representation of the PAH spectrum which is critical for interpreting the LW3 fluxes. In the Elbaz's et al analysis We report in Fig.…”

Section: Estimating the Rate Of Ongoing Star Formationmentioning

confidence: 99%

“…However, dusty starbursts show occasional evidence in the starburst regions for the presence of younger red supergiants as shown by the pronounced [CO] 2.3 µm absorption (e.g. Foerster-Schreiber et al 2001). Obviously, a contribution by such young massive stars, even heavily extinguished, would substantially decrease the M/L in the near-IR, hence affecting the stellar mass estimate.…”

Section: Estimating the Baryonic Massesmentioning

confidence: 99%

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Infrared spectroscopy of faint 15 μm sources in the Hubble Deep Field South: First hints at the properties of the sources of the IR background

Franceschini

Berta

Rigopoulou

et al. 2003

A&A

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Abstract. We present a spectroscopic analysis of a sample of 21 galaxies with z = 0.2−1.5 drawn from a 25 square arcmin ultradeep ISOCAM survey at λ eff = 15 µm centered in the WFPC-2 Hubble Deep Field South. Near-infrared spectra are reported for 18 ISO sources, carried out with ISAAC on the VLT, aimed at detecting the redshifted H α + [N]. Additional optical data come from the ESO VLT/FORS2 and NTT/EMMI, primarily targeting [O], [O] and H β for further physical insight. Although not numerous in terms of areal density in the sky, this population of very luminous IR sources has been recently found to be responsible for a substantial fraction of the extragalactic background light energy density. H α line emission is detected in virtually all the observed objects down to a flux limit of 7 × 10 −17 erg cm −2 s −1 (corresponding to L Hα > 10 41 erg s −1 at z = 0.6 for H 0 = 65, Ω Λ = 0.7 and Ω m = 0.3). Our analysis (including emission line, morphology, and SED properties) shows clear evidence for AGN activity in only two of these sources: one type-I (with broadened H α at z = 1.57) and one type-II quasars (with inverted [N]/H α ratio at z = 1.39), while we suspect the presence of an AGN in two further sources (an Ultra-Luminous IR Galaxy, ULIRG, at z = 1.27 and a luminous galaxy at z = 0.69). The H α luminosities indicate star formation rates (S FR) in the remaining sources between 0.5 and 20 M /yr, assuming a Salpeter IMF between 0.1 and 100 M and without extinction corrections. We find good correlations between the mid-IR, the radio and H α luminosities, confirming the mid-IR light as a good tracer of star formation (while the S FR based on H α flux show some large scatter and offset, which are still to be understood). We have estimated the baryonic masses in stars with a newly-developed tool fitting the overall optical-IR continuum, and found that the host galaxies of ISO sources are massive members of groups with typically high rates of SF (S FR ∼ 10 to 300 M /yr). We have finally compared this ongoing SF activity with the already formed stellar masses to estimate the timescales t SF for the stellar build-up, which turn-out to be widely spread in these objects between 0.1 Gyrs to more than 10 Gyr. The faint ISOCAM galaxies appear to form a composite population, including moderately active but very massive spiral-like galaxies, and very luminous ongoing starbursts, in a continuous sequence. From the observed t SF and assuming typical starburst timescales, we infer that, with few exceptions, only a fraction of the galactic stars can be formed in any single starburst event, while several of such episodes during a protracted SF history are required for the whole galactic build-up.

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Section: Estimating the Rate Of Ongoing Star Formationmentioning

confidence: 99%

Section: Estimating the Baryonic Massesmentioning

confidence: 99%

Infrared spectroscopy of faint 15 μm sources in the Hubble Deep Field South: First hints at the properties of the sources of the IR background

Franceschini

Berta

Rigopoulou

et al. 2003

A&A

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“…4.4.1. See also discussion in Förster-Schreiber et al 2001). For all three elements, the major ionisation stages found in H II regions are covered by the ISO-SWS spectra, which minimises the required ionisation correction factors.…”

Section: Introductionmentioning

confidence: 99%

A mid-infrared spectroscopic survey of starburst galaxies: Excitation and abundances

Verma¹,

Lutz²,

Sturm³

et al. 2003

A&A

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133

236

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Abstract. We present spectroscopy of mid-infrared emission lines in twelve starburst regions, located in eleven starburst galaxies, for which a significant number of lines between 2.38 and 45 µm were observed with the ISO Short Wavelength Spectrometer, with the intention of providing a reference resource for mid-infrared spectra of starburst galaxies. The observation apertures were centred on actively star forming regions, including those which are inaccessible at optical wavelengths due to high levels of obscuration. We use this data set, which includes fine structure and hydrogen recombination lines, to investigate excitation and to derive gas phase abundances of neon, argon, and sulphur of the starburst galaxies. The derived Ne abundances span approximately an order of magnitude, up to values of ∼3 times solar. The excitation ratios measured from the Ne and Ar lines correlate well with each other (positively) and with abundances (negatively). Both in excitation and abundance, a separation of objects with visible Wolf-Rayet features (high excitation, low abundance) is noted from those without (low excitation, high abundance). For a given abundance, the starbursts are of relatively lower excitation than a comparative sample of H II regions, possibly due to ageing stellar populations. By considering the abundance ratios of S with Ne and Ar we find that, in our higher metallicity systems, S is relatively underabundant by a factor of ∼3. We discuss the origin of this deficit and favour depletion of S onto dust grains as a likely explanation. This weakness of the mid-infrared fine structure lines of sulphur has ramifications for future infrared missions such as SIRTF and Herschel since it indicates that the S lines are less favourable tracers of star formation than is suggested by nebular models which do not consider this effect. In a related paper (Sturm et al. 2002), we combine our results with spectra of Seyfert galaxies in order to derive diagnostic diagrams which can effectively discriminate between the two types of activity in obscured regions on the basis of excitation derived from detected mid-infrared lines.

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“…The high ISM pressure is supplied by hot gas (kT ∼ 0.7-0.9kev) that pervades the region around the main starburst clumps. The structure of the ISM in M82 thus is quite different from that in the Milky Way's disk (see also Förster-Schreiber et al 2001, 2003.…”

Section: Cymcs and Starburst Clumps In M82mentioning

confidence: 99%

“…Taking full advantage of the opportunities opened by AO on ELTs in the near infrared will require continued preparatory work on infrared properties of stellar populations covering a range in age. Much of the necessary data can be obtained in the Local Group using existing telescopes, providing an excellent starting point for spectroscopic surveys of key infrared spectroscopic characteristics of SSPs and composite stellar populations (Förster-Schreiber et al 2001, 2003.…”

Section: Opportunities For Extremely Large Telescopesmentioning

confidence: 99%

Exploring starburst astrophysics with ELTs

Gallagher¹,

Smith

2005

Proc. IAU

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Abstract. Star formation in starbursts produces compact star clusters which extend in mass up to the super star clusters (SSCs) which resemble young globular clusters. Compact young massive star clusters (cYMCs) in turn cluster along with other young stars into starburst clumps. Using M82 as an example we briefly review how the presence of starburst clumps affects the evolution of the host galaxy. Extremely large telescopes (ELTs) will be essential for understanding how starburst clumps and their constituent star clusters evolve. In nearby systems their combination of sensitivity and angular resolution will allow us to explore the structures, kinematics, and abundances of cYMCs. For systems at cosmological distances the high surface brightnesses of the starburst clumps makes them prime gateways for exploring the early evolution of galaxies.

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Near‐Infrared Integral Field Spectroscopy and Mid‐Infrared Spectroscopy of the Starburst Galaxy M82

Cited by 127 publications

References 124 publications

Infrared spectroscopy of faint 15 μm sources in the Hubble Deep Field South: First hints at the properties of the sources of the IR background

Infrared spectroscopy of faint 15 μm sources in the Hubble Deep Field South: First hints at the properties of the sources of the IR background

A mid-infrared spectroscopic survey of starburst galaxies: Excitation and abundances

Exploring starburst astrophysics with ELTs

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