High Spatial Resolution Fabry-Perot Imaging of M82: Near-Infrared Recombination Line Observations

Satyapal, S.; Watson, D. M.; Pipher, J. L.; Forrest, W. J.; Coppenbarger, D.; Raines, S. N.; Libonate, S.; Piche, Francois; Greenhouse, Matthew A.; Smith, H. A.; Thompson, K. L.; Fischer, J.; Woodward, C. E.; Hodge, T. M.

doi:10.1086/175990

Cited by 48 publications

(62 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…From their Figure 5, we estimate that the upper limit to the contribution of the nucleus is 200 mJy, which corresponds to one contour spacing in their Ðgure. The foreground extinction was estimated using Telesco et al (1991) and Satyapal et al (1995). M82 shows variable hard X-ray Ñux (Ptak & Griffiths 1999 ;Matsumoto & Tsuru 1999), which led these authors to speculate about whether M82 might be harboring an AGN.…”

Section: Appendix Amentioning

confidence: 99%

N‐Band Imaging of Seyfert Nuclei and the Mid‐Infrared–X‐Ray Correlation

Krabbe¹,

Maiolino²

2001

ApJ

111

118

View full text Add to dashboard Cite

We present new mid-infrared (N-band) images of a sample of eight nearby Seyfert galaxies. In all of our targets, we detect a central unresolved source, which in some cases has been identiÐed for the Ðrst time. In particular, we have detected the mid-infrared emission from the active nucleus of NGC 4945, which previously remained undetected at any wavelength but hard X-rays. We also detect circumnuclear extended emission in the Circinus galaxy along its major axis and Ðnd marginal evidence for extended circumnuclear emission in NGC 3281. The high spatial resolution of our data allows us to separate (1A .7) the Ñux of the nuclear point sources from the extended circumnuclear starburst (if present). We complement our sample with literature data for a number of nonactive starburst galaxies and relate the nuclear N-band Ñux to published hard (2È10 keV) X-ray Ñuxes. We Ðnd tight and well-separated correlations between the nuclear N-band Ñux and X-ray Ñux for both Seyfert and starburst nuclei that span over 3 orders of magnitude in luminosity. We demonstrate that these correlations can be used as a powerful classiÐcation tool for galactic nuclei. For example, we Ðnd strong evidence against NGC 1808 currently harboring an active Seyfert nucleus based on its position in the mid-infraredÈX-ray diagram. On the other hand, we conÐrm that NGC 4945 is in fact a Seyfert 2 galaxy.

show abstract

Section: Appendix Amentioning

confidence: 99%

N‐Band Imaging of Seyfert Nuclei and the Mid‐Infrared–X‐Ray Correlation

Krabbe¹,

Maiolino²

2001

ApJ

111

118

View full text Add to dashboard Cite

show abstract

“…Although the dust provides the raw material for the clusters' formation, it also obscures and reradiates most of the light from the Article published by EDP Sciences starburst in the infrared (Keto et al 2005). However, despite all the bright sources associated with the active starburst core suffering from such heavy extinction (in the range A V ∼ 5-25 mag; e.g., Telesco et al 1991;McLeod et al 1993;Satyapal et al 1995;Mayya et al 2008, and references therin), many individual clusters remain bright enough to obtain good photometry and spectroscopy for (see, for example, Smith et al 2006;McCrady & Graham 2007).…”

Section: Introductionmentioning

confidence: 99%

Star cluster versus field star formation in the nucleus of the prototype starburst galaxy M 82

Barker

Grijs

Cerviño³

2008

A&A

View full text Add to dashboard Cite

We analyse high-resolution Hubble Space Telescope/Advanced Camera for Surveys imaging of the nuclear starburst region of M 82, obtained as part of the Hubble Heritage mosaic made of this galaxy, in four filters (Johnson-Cousins equivalent B, V, and I broad bands, and an Hα narrow-band filter), as well as subsequently acquired U-band images. We find a complex system of ∼150 star clusters in the inner few 100 pc of the galaxy. We do not find any conclusive evidence of a cluster-formation epoch associated with the most recent starburst event, believed to have occurred about 4-6 Myr ago. This apparent evidence of decoupling between cluster and field-star formation is consistent with the view that star cluster formation requires special conditions. However, we strongly caution, and provide compelling evidence, that the "standard" simple stellar population analysis method we have used significantly underestimates the true uncertainties in the derived ages due to stochasticity in the stellar initial mass function and the corresponding sampling effects.

show abstract

“…He also suggested that extinction corrections in M82 made by others were too high, and this made it appear like M82 had a truncated IMF when really it didn't. Satyapal (1995) indeed found low extinction in M82 from Paβ/Brγ, which gave A V = 2 − 12 mag compared to 25 mag in Rieke et al (1980). Satyapal then got a K-band luminosity 3 times lower than Rieke et al, and saw no need for IMF truncation.…”

Section: Introduction: History Of Starburst Imfsmentioning

confidence: 82%

The Initial Mass Function in Starbursts

Elmegreen

2005

Starbursts

View full text Add to dashboard Cite

The history of the IMF in starburst regions is reviewed. The IMFs are no longer believed to be top-heavy, although some superstar clusters, whether in starburst regions or not, could be. Introduction: History of Starburst IMFsEarly starburst observations suggested the luminous mass from young massive stars is comparable to the dynamical mass from the rotation curve (see reviews in Telesco 1988; Scalo 1990; Zinnecker 1996; Leitherer 1999). This implied there was a deficit in low mass stars. The nearby starburst galaxy, M82, was one of the best cases. Rieke et al. (1980Rieke et al. ( , 1993 modeled M82's gas mass, luminous star mass, rotation curve mass, 2.2 µm flux, Lyman continuum flux, CO index for supergiants, and the Brα/Brγ ratio, giving an extinction A V = 25 mag. They concluded that only the usual IMF models with lower mass limits M L > 3 − 6 M ⊙ worked. Kronberg et al. (1985) used the Lyman continuum flux from radio emission in M82 to determine the star formation rate, and used the total gas mass combined with an efficiency estimate to conclude that the IMF is top-heavy compared to the Miller & Scalo (1979) IMF. Bernlohr (1992 fit the same M82 properties as Rieke et al., plus the heavy element abundance and FIR line ratios, and concluded that either the IMF slope is shallower than the Scalo (1986) IMF by 1, or there is a lower mass cutoff greater than 1.5-2

show abstract

High Spatial Resolution Fabry-Perot Imaging of M82: Near-Infrared Recombination Line Observations

Cited by 48 publications

References 0 publications

N‐Band Imaging of Seyfert Nuclei and the Mid‐Infrared–X‐Ray Correlation

N‐Band Imaging of Seyfert Nuclei and the Mid‐Infrared–X‐Ray Correlation

Star cluster versus field star formation in the nucleus of the prototype starburst galaxy M 82

The Initial Mass Function in Starbursts

Contact Info

Product

Resources

About