University of Hertfordshire

From the same journal

From the same journal

By the same authors

A low H I column density filament in NGC 2403: signature of interaction or accretion

Research output: Contribution to journalArticlepeer-review


  • 1407.3648v1

    Accepted author manuscript, 3.7 MB, PDF document

  • W.J.G. de Blok
  • K.M. Keating
  • D.J. Pisano
  • F. Fraternali
  • F. Walter
  • T. Oosterloo
  • E. Brinks
  • F. Bigiel
  • A. Leroy
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Original languageEnglish
Article numberA68
Number of pages11
JournalAstronomy and Astrophysics
Publication statusPublished - 25 Sep 2014


Observed H i accretion around nearby galaxies can only account for a fraction of the gas supply needed to sustain the currently observed star formation rates. It is possible that additional accretion occurs in the form of low column density cold flows, as predicted by numerical simulations of galaxy formation. To constrain the presence and properties of such flows, we present deep H i observations obtained with the NRAO Green Bank Telescope of an area measuring 4° × 4° around NGC 2403. These observations, with a 5σ detection limit of 2.4 × 1018 cm-2 over a 20 km s-1 linewidth, reveal a low column density, extended cloud outside the main H i disk, about 17′ (~ 16 kpc or ~ 2 R25) to the NW of the center of the galaxy. The total H i mass of the cloud is 6.3 × 106 M⊙, or 0.15 percent of the total H i mass of NGC 2403. The cloud is associated with an 8 kpc anomalous-velocity H i filament in the inner disk, that was previously observed in deep VLA observations. We discuss several scenarios for the origin of the cloud, and conclude that it is either accreting from the intergalactic medium, or is the result of a minor interaction with a neigboring dwarf galaxy


Date of acceptance: 12/07/2014


ID: 7789464