VLBI Images of 49 Radio Supernovae in Arp 220

Lonsdale, Colin J.; Diamond, P. J.; Thrall, H.; Smith, H. E.; Lonsdale, C. J.

doi:10.1086/505193

Cited by 164 publications

(246 citation statements)

References 32 publications

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“…4 ‫ע‬ 2 indicates an SFR high enough to power its entire IR luminosity (Lonsdale et al 2006). These studies confirm that CCSN rates a couple of orders of magnitude higher than in ordinary field galaxies can be expected for starburst-dominated (U)LIRGs.…”

supporting

confidence: 63%

Radio Detection of Supernova 2004ip in the Circumnuclear Region of the Luminous Infrared Galaxy IRAS 18293-3413

Pérez-Torres

Mattila

Alberdi

et al. 2007

ApJ

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We report a radio detection of supernova SN 2004ip in the circumnuclear region of the luminous infrared galaxy IRAS 18293Ϫ3413 , using Very Large Array (VLA) observations at 8.4 GHz on 2007 June 11. SN 2004ip had been previously discovered at near-infrared wavelengths using adaptive optics observations, but its nature (core collapse or thermonuclear) could not be definitely established. Our radio detection, about 3 years after the explosion of the supernova, indicates a prominent interaction of the ejecta of SN 2004ip with the circumstellar medium, confirming that the supernova was a core collapse event (probably a Type II) and strongly suggesting that its progenitor was a massive star with a significant mass loss prior to its explosion. SN 2004ip has a 8.4 GHz luminosity of ergs s Hz , about 3 times as bright as SN 2000ft in NGC 7469 at a 27 Ϫ1 Ϫ13.5 # 10 similar age; given its projected distance to the nucleus (∼500 pc), it is one of the closest of all known radio SNe to a galaxy nucleus and one of the brightest radio SNe ever.

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supporting

confidence: 63%

Radio Detection of Supernova 2004ip in the Circumnuclear Region of the Luminous Infrared Galaxy IRAS 18293-3413

Pérez-Torres

Mattila

Alberdi

et al. 2007

ApJ

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“…Sa8 indicates that the luminosity from the Arp 220 western nucleus could be generated by 200−1000 super-star clusters. An important contribution from star formation to the luminosity of the western nucleus is indeed evident (e.g., Smith et al 1998;Lonsdale et al 2006), and the apparent lack of strong X-ray emission from X-ray binaries associated with star formation (Lonsdale et al 2006) can be interpreted in terms of extreme absorption column densities (Sa08, this work).…”

Section: Sources Of Luminositymentioning

confidence: 94%

Herschel/PACS spectroscopy of NGC 4418 and Arp 220: H₂O, H₂¹⁸O, OH,¹⁸OH, O I, HCN, and NH₃

González-Alfonso

Fischer

Graciá-Carpio

et al. 2012

A&A

157

166

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Full range Herschel/PACS spectroscopy of the (ultra)luminous infrared galaxies NGC 4418 and Arp 220, observed as part of the SHINING key programme, reveals high excitation in H 2 O, OH, HCN, and NH 3 . In NGC 4418, absorption lines were detected with E lower > 800 K (H 2 O), 600 K (OH), 1075 K (HCN), and 600 K (NH 3 ), while in Arp 220 the excitation is somewhat lower. While outflow signatures in moderate excitation lines are seen in Arp 220 as have been seen in previous studies, in NGC 4418 the lines tracing its outer regions are redshifted relative to the nucleus, suggesting an inflow withṀ 12 M yr −1 . Both galaxies have compact and warm (T dust 100 K) nuclear continuum components, together with a more extended and colder component that is much more prominent and massive in Arp 220. A chemical dichotomy is found in both sources: on the one hand, the nuclear regions have high H 2 O abundances, ∼10 −5 , and high HCN/H 2 O and HCN/NH 3 column density ratios of 0.1−0.4 and 2−5, respectively, indicating a chemistry typical of evolved hot cores where grain mantle evaporation has occurred. On the other hand, the high OH abundance, with OH/H 2 O ratios of ∼0.5, indicates the effects of X-rays and/or cosmic rays. The nuclear media have high surface brightnesses ( 10 13 L /kpc 2 ) and are estimated to be very thick (N H 10 25 cm −2 ). While NGC 4418 shows weak absorption in H 18 2 O and 18 OH, with a 16 O-to-18 O ratio of 250−500, the relatively strong absorption of the rare isotopologues in Arp 220 indicates 18 O enhancement, with 16 O-to-18 O of 70−130. Further away from the nuclear regions, the H 2 O abundance decreases to 10 −7 and the OH/H 2 O ratio is reversed relative to the nuclear region to 2.5−10. Despite the different scales and morphologies of NGC 4418, Arp 220, and Mrk 231, preliminary evidence is found for an evolutionary sequence from infall, hot-core like chemistry, and solar oxygen isotope ratio to high velocity outflow, disruption of the hot core chemistry and cumulative high mass stellar processing of 18 O.

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“…These authors interpret their results as a ∼100 km s −1 outflow driven by supernova explosions (or radiation pressure from the starburst). As many as 49 supernova remnants (SNRs) have been detected with VLBI (1 pc resolution) at 18 cm (Lonsdale et al 2006), confirming the formation and demise of many massive stars. The latter authors derive a supernova rate of 3 yr −1 for the western nucleus and 1 yr −1 for the eastern nucleus, more than two orders of magnitude larger than the entire Milky Way.…”

Section: Introductionmentioning

confidence: 94%

Star formation in extreme environments: the effects of cosmic rays and mechanical heating

Meijerink

Spaans²,

Loenen

et al. 2010

A&A

168

209

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Context. The molecular interstellar medium in extreme environments, such as Arp 220, but also NGC 253 appears to have extremely high cosmic ray (CR) rates (10 3 −10 4 × Milky Way) and substantial mechanical heating from supernova driven turbulence. Aims. We explore the consequences of high CR rates and mechanical heating on the chemistry of the clouds. Methods. PDR model predictions are made for low, n = 10 3 , and high, n = 10 5.5 cm −3 , density clouds using well-tested chemistry and radiation transfer codes. Column densities of relevant species are discussed, and special attention is given to water-related species. Fluxes are shown for fine-structure lines of O, C + , C, and N + , and molecular lines of CO, HCN, HNC, and HCO + . A comparison is made with an X-ray dominated region model. Results. Fine-structure lines of [CII], [CI], and [OI]are remarkably similar for different mechanical heating and CR rates, when already exposed to large amounts of UV. Both HCN and H 2 O abundances are boosted for very high mechanical heating rates, while ionized species are relatively unaffected. Both OH + and H 2 O + are enhanced for very high CR rates ζ ≥ 5 × 10 −14 s −1 . A combination of OH + , OH, H 2 O + , H 2 O, and H 3 O + traces the CR rates, and is able to distinguish between enhanced cosmic rays and X-rays.

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VLBI Images of 49 Radio Supernovae in Arp 220

Cited by 164 publications

References 32 publications

Radio Detection of Supernova 2004ip in the Circumnuclear Region of the Luminous Infrared Galaxy IRAS 18293-3413

Radio Detection of Supernova 2004ip in the Circumnuclear Region of the Luminous Infrared Galaxy IRAS 18293-3413

Herschel/PACS spectroscopy of NGC 4418 and Arp 220: H₂O, H₂¹⁸O, OH,¹⁸OH, O I, HCN, and NH₃

Star formation in extreme environments: the effects of cosmic rays and mechanical heating

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VLBI Images of 49 Radio Supernovae in Arp 220

Cited by 164 publications

References 32 publications

Radio Detection of Supernova 2004ip in the Circumnuclear Region of the Luminous Infrared Galaxy IRAS 18293-3413

Radio Detection of Supernova 2004ip in the Circumnuclear Region of the Luminous Infrared Galaxy IRAS 18293-3413

Herschel/PACS spectroscopy of NGC 4418 and Arp 220: H2O, H218O, OH,18OH, O I, HCN, and NH3

Star formation in extreme environments: the effects of cosmic rays and mechanical heating

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About

Herschel/PACS spectroscopy of NGC 4418 and Arp 220: H₂O, H₂¹⁸O, OH,¹⁸OH, O I, HCN, and NH₃