We have imaged the H92alpha (8.3 GHz), H75alpha (15 GHz), and H166alpha (1.4
GHz) Radio Recombination Lines (RRLs) from NGC 253 at resolutions of 4.5 pc
(0.4"), 2.5 pc (0.2") and 53 pc (4.5") respectively. The H92alpha line arises
from individual compact sources, most of which possess radio continuum
counterparts. The line widths range from ~200 km/s for the sources near the
radio nucleus to 70-100 km/s for the extranuclear ones. These lines are emitted
by gas at a density ~10000 /cc. The remainder of the cm-wave RRLs arise in
lower density gas (~500 /cc) with a higher area filling factor and with ten
times highermass. A third component of higher density gas (>10000 /cc) is
required to explain the mm-wave RRLs.Comment: Accepted by A&A; Changed to fit all figures within pag

Anantharamaiah

Antonucci

Böker

Carilli

Carlstrom

Dyson

Engelbracht

Forbes

Genzel

Goss

Holtzman

K. R. Anantharamaiah

Kalas

Keto

Kotilainen

Lizano

Mebold

Meurer

Mohan

Niruj R. Mohan

Paglione

Payne

Peng

Piña

Puxley

Salem

Seaquist

Shaver

Telesco

Turner

Ulvestad

W. M. Goss

Walmsley

Weaver

English

arXiv

We have imaged the H92α (8.3 GHz), H75α (15 GHz), and H166α (1.4 GHz) Radio Recombination Lines (RRLs) from NGC 253 at resolutions of 4.5 pc (0.4'') , 2.5 pc (0.2'') and 53 pc (4.5'') respectively. The H92α line arises from individual compact sources, most of which possess radio continuum counterparts. The line widths range from ~200 km s-1 for the sources near the radio nucleus to 70-100 km s-1 for the extranuclear ones. These lines are emitted by gas at a density ~104 cm-3. The remainder of the cm-wave RRLs arise in lower density gas (~500 cm-3) with a higher area filling factor and with ten times higher mass. A third component of higher density gas (〉104 cm-3) is required to explain the mm-wave RRLs.

Appendix A is only available in electronic form at http://www.edpsciences.or

Mohan, Niruj R.

Goss, W.M.

Anantharamaiah, K.R.

Raman Research Institute Digital Repository

Astronomy and Astrophysics

Multi-density model of the ionised gas in NGC 253 using radio recombination lines

We have imaged the H92alpha (8.3 GHz), H75alpha (15 GHz), and H166alpha (1.4 GHz) Radio Recombination Lines (RRLs) from NGC 253 at resolutions of 4.5 pc (0.4"), 2.5 pc (0.2") and 53 pc (4.5") respectively. The H92a line arises from individual compact sources, most of which possess radio continuum counterparts. The line widths range from similar to 200 km s(-1) for the sources near the radio nucleus to 70 - 100 km s(-1) for the extranuclear ones. These lines are emitted by gas at a density similar to 10(4) cm(-3). The remainder of the cm-wave RRLs arise in lower density gas (similar to500 cm(-3)) with a higher area filling factor and with ten times higher mass. A third component of higher density gas (> 10(4) cm(-3)) is required to explain the mm-wave RRLs

Mohan, Niruj R

Goss, WM

Anantharamaiah, KR

Open Access Repository of IISc Research Publications

Name not available

International audienceWe have imaged the H92α (8.3 GHz), H75α (15 GHz), and H166α (1.4 GHz) Radio Recombination Lines (RRLs) from NGC 253 at resolutions of 4.5 pc (0.4'') , 2.5 pc (0.2'') and 53 pc (4.5'') respectively. The H92α line arises from individual compact sources, most of which possess radio continuum counterparts. The line widths range from ~200 km s-1 for the sources near the radio nucleus to 70-100 km s-1 for the extranuclear ones. These lines are emitted by gas at a density ~104 cm-3. The remainder of the cm-wave RRLs arise in lower density gas (~500 cm-3) with a higher area filling factor and with ten times higher mass. A third component of higher density gas (>104 cm-3) is required to explain the mm-wave RRLs. Appendix A is only available in electronic form at http://www.edpsciences.or

Goss, W. M.

Anantharamaiah, K. R.

HAL-INSU

We have imaged the H92&#945; (8.3 GHz), H75&#945; (15 GHz), and H166&#945; (1.4 GHz) Radio Recombination Lines (RRLs) from NGC 253 at resolutions of 4.5 pc (0.4" ) , 2.5 pc (0.2" ) and 53 pc (4.5" ) respectively. The H92&#945; line arises from individual compact sources, most of which possess radio continuum counterparts. The line widths range from ~200 km s -1 for the sources near the radio nucleus to 70-100 km s -1 for the extranuclear ones. These lines are emitted by gas at a density ~10 4 cm -3. The remainder of the cm-wave RRLs arise in lower density gas (~500 cm -3) with a higher area filling factor and with ten times higher mass. A third component of higher density gas ( &gt;10 4 cm -3) is required to explain the mm-wave RRLs

Publications of the IAS Fellows

We have imaged the H92α  (8.3 GHz), H75α  (15 GHz), and H166α (1.4 GHz) Radio Recombination 
Lines (RRLs) from NGC 253 at resolutions of 4.5 pc (0.4″) , 2.5 pc (0.2″) and 53 pc 
(4.5″) respectively. The H92α  line
arises from individual compact sources, most of which possess radio continuum counterparts. The line widths
range from ~200 km s-1  for the sources near the radio nucleus to 70–100 km s-1  for the extranuclear
ones. These lines are emitted by gas at a density ~104 cm-3. The remainder of the cm-wave RRLs
arise in lower density gas (~500 cm-3) with a higher area filling factor and with ten times higher
mass. A third component of higher density gas (>104 cm-3) is required to explain the mm-wave RRLs

EDP Sciences OAI-PMH repository (1.2.0)

Multi-density model of the ionised gas in NGC 253 using radio recombination lines

Crossref

Indian Academy of Sciences

Multi-density model of the ionised gas in NGC 253 using radio
  recombination lines

Multi-density model of the ionised gas in NGC 253 using radio recombination lines

Abstract

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Raman Research Institute Digital Repository

Open Access Repository of IISc Research Publications

Name not available

HAL-INSU

Publications of the IAS Fellows

EDP Sciences OAI-PMH repository (1.2.0)

Crossref

Indian Academy of Sciences

Raman Research Institute Digital Repository