Statistics variations of the quality of visible images

Hecquet, J.; Coupinot, G.; Futaully, R.

doi:10.1088/0150-536x/18/3/002

Cited by 6 publications

(18 citation statements)

References 9 publications

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“…Similarly, the radio supernova reported by Heeschen et al (1983) and Yin (1994), which from Figs. 1, 2 and 8 of this paper clearly corresponds to H α source 14 of Hecquet et al (1987), only falls at that location subject to the above adjustment of the astrometry of Hecquet et al (1987). The astrometry of Casini, Heeschen et al (1983), Yin (1994) and Deeg et al (1993) appears to be mutually consistent with all recent imaging data.…”

Section: A Hidden Sourcesupporting

confidence: 75%

“…(We stress, by the way, that this source is clearly distinguished also in the un-deconvolved maps.) Hecquet et al (1987) reported numerous optical emission knots in Mkn 297, and knots 7 and 8 in their numbering scheme have the second and third highest values of B − R (1.8 and 2.3 respectively) for the system and are within a few arcseconds of the mid-infrared peak. Knot 14 is the site of the variable radio source reported by Heeschen et al (1983).…”

Section: A Hidden Sourcementioning

confidence: 99%

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ISO observations of the interacting galaxy Markarian 297

Metcalfe

O’Halloran

McBreen

et al. 2005

A&A

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Markarian (Mkn) 297 is a complex system comprised of two interacting galaxies that has been modelled with a variety of scenarios. Observations of this system were made with the Infrared Space Observatory (ISO) using the ISOCAM, ISOPHOT and LWS instruments. ISOCAM maps at 6.7 µm, 7.7 µm, 12 µm and 14.3 µm are presented which, together with PHT-S spectrometry of the central interacting region, probe the dust obscured star formation and the properties of the organic dust. The ISOCAM observations reveal that the strongest emission in the four bands is at a location completely unremarkable at visible and near-IR (e.g. 2MASS) wavelengths, and does not coincide with the nuclear region of either colliding galaxy. This striking characteristic has also been observed in the overlap region of the colliding galaxies in the Antennae (NGC 4038/4039), the intragroup region of Stephan's Quintet, and in IC 694 in the interacting system Arp 299, and again underlines the importance of infrared observations in understanding star formation in colliding/merging systems. At 15 µm, the hidden source in Mkn 297 is, respectively, 14.6 and 3.8 times more luminous than the hidden sources in the Antennae (NGC 4038/4039) and Stephan's Quintet. Numerical simulations of the Mkn 297 system indicate that a co-planar radial penetration between two disk galaxies yielded the observed wing formation in the system about 1.5 × 10 8 years after the collision. A complex emission pattern with knots and ridges of emission was detected with ISOCAM. The 7.7 µm map predominantly shows the galaxy in emission from the 7.7 µm feature attributed to PAHs (Polycyclic Aromatic Hydrocarbons). The 14.3/7.7 µm ratio is greater than unity over most of the galaxy, implying widespread strong star formation. Strong emission features were detected in the ISOPHOT spectrum, while [O I], [O III] and [C II] emission lines were seen with LWS. Using data from the three instruments, luminosities and masses for two dust components were determined. The total infrared luminosity is approximately 10 11 L , which (marginally) classifies the system as a luminous infrared galaxy (LIRG). A supernova that exploded in 1979 (SN 1982aa) gave rise to one of the most powerful known radio remnants which falls close to the strongest mid-infrared source and is identified with star forming region 14 in the optical. This supernova explosion may have been accompanied by a gamma-ray burst (GRB), consistent with the idea that GRBs are associated with supernovae in star forming regions, and a search for a GRB consistent with the direction to Mkn 297, in satellite data from July to December 1979, is recommended.

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Section: A Hidden Sourcesupporting

confidence: 75%

Section: A Hidden Sourcementioning

confidence: 99%

ISO observations of the interacting galaxy Markarian 297

Metcalfe

O’Halloran

McBreen

et al. 2005

A&A

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“…4) re sembles that of a BCD of type iE, its luminosity (M b = -20.4) is brighter than the luminosity cutoff of Mb = -18 (Thuan & Martin 1981) and it is not a bona-fide dwarf galaxy. Hecquet et al (1987) have resolved the central re gion in ~ 40 knots, one of them coinciding with the strong radio source Mrk297A (Heeschen et al 1983). Spectro scopic observations (Alloin & Dufflot 1979) revealed two kinematically decoupled components, giving circumstan tial evidence for the interpretation that Mkn 297 is a dy namically perturbed system (Taniguchi & Noguchi 1991).…”

Section: Sample Descriptionmentioning

confidence: 91%

Optical structure and star formation in blue compact dwarf galaxies. I. Observations and profile decomposition

Papaderos

Loose

Thuan

et al. 1996

Astron. Astrophys. Suppl. Ser.

233

321

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Abstract. -We present new B and R CCD surface photometry for a sample of 4 Blue Compact Dwarf Galaxies (BCDs) and 2 higher luminosity starburst galaxies. We find that the BCD surface brightness profiles (SBPs) can be generally well fitted by the sum of the light of 3 distinct components: 1) an exponential component at large radii, with or without a central flattening which describes the underlying older stellar population; 2) a plateau component at intermediate radii and 3) a gaussian component at small radii. The last 2 components describe the ongoing starburst superimposed on the older stellar component. We apply the 3-component decomposition scheme to 8 more BCDs from the literature and, for the total sample of 14 galaxies, derive structural properties such as central surface brightness and scale length, and perform a deprojection to obtain the luminosity density distribution for each component. We also derive B -R color profiles and find that BCDs show generally a reddening outwards, followed by a blueing beyond a transition radius.

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“…To better distinguish between the two leading hypotheses for cluster formation in NGC 1275, and to try to find more young compact massive clusters, we observed several inter- (Lutz 1991), although ground-based resolution is not sufficient to determine whether these clusters are as compact as globulars. NGC 6052 has also been observed to have bright blue knots (Hequet et al 1987). The central galaxies in Abell 1795, Abell 496, Abell 2029, and Abell 2597 were also observed; these clusters are among those with the largest inferred mass inflow rates from x-ray observations (Fabian 1992).…”

mentioning

confidence: 94%

Star Clusters in Interacting and Cooling Flow Galaxies

Holtzman¹,

Watson²,

Mould³

et al. 1996

The Astronomical Journal

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Two interacting galaxies and four central galaxies in cooling flow clusters were observed with the Hubble Space Telescope to look for young compact massive star clusters. The two interacting galaxies, NGC 3597 and NGC 6052, show clear evidence for resolved bright blue clusters that are likely to be comparable in mass to Galactic globulars based on their colors and brightnesses. In NGC 3597, the clusters have physical sizes comparable to Galactic globulars. In NGC 6052, there are a few compact clusters, but most appear more extended. No such objects were seen in three of the four cooling flow galaxies. The central galaxy in Abell 1795 may have several massive blue clusters, but its distance prevents us from knowing how compact they are.

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Statistics variations of the quality of visible images

Cited by 6 publications

References 9 publications

ISO observations of the interacting galaxy Markarian 297

ISO observations of the interacting galaxy Markarian 297

Optical structure and star formation in blue compact dwarf galaxies. I. Observations and profile decomposition

Star Clusters in Interacting and Cooling Flow Galaxies

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