TY - JOUR
T1 - Evolution of the 1919 ejecta of V605 aquilae
AU - Clayton, Geoffrey C.
AU - Bond, Howard E.
AU - Long, Lindsey A.
AU - Meyer, Paul I.
AU - Sugerman, Ben E K
AU - Montiel, Edward
AU - Sparks, William B.
AU - Meakes, M. G.
AU - Chesneau, O.
AU - De Marco, O.
N1 - Copyright 2013 The American Astronomical Society. First published in the Astrophysical journal, 771(2), 130, 2013, published by IOP Publishing. The original publication is available at http://www.doi.org/10.1088/0004-637X/771/2/130. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.
PY - 2013/7/10
Y1 - 2013/7/10
N2 - New imaging of V605 Aql, was obtained in 2009 with HST/WFPC2, which had a nova-like outburst in 1919, and is located at the center of the planetary nebula (PN), A58. This event has long been ascribed to a final helium shell flash, but it has been suggested recently that it may instead have been an ONe nova. The new images provide an 18 yr baseline for the expansion of the ejecta from the 1919 event. In addition, the central star has been directly detected in the visible for the first time since 1923, when it faded from sight due to obscuration by dust. The expansion of the ejecta has a velocity of ∼200 km s-1, and an angular expansion rate of ∼10 mas yr-1, consistent with a 1919 ejection. This implies a geometric distance of 4.6 kpc for V605 Aql, consistent with previous estimates. The gas mass in the central knot of ejecta was previously estimated to be 5 × 10-5 M. It is estimated that warm dust associated with this gas has a mass of ∼10 -5 M. There is also evidence for a significant amount, 10 -3 M, of cold (75 K) dust, which may be associated with its PN. The knot ejected in 1919 is asymmetrical and is approximately aligned with the asymmetry of the surrounding PN. Polarimetric imaging was obtained to investigate whether the 2001 spectrum of V605 Aql was obtained primarily in scattered light from dust in the central knot, but the signal-to-noise in the data was insufficient to measure the level of polarization.
AB - New imaging of V605 Aql, was obtained in 2009 with HST/WFPC2, which had a nova-like outburst in 1919, and is located at the center of the planetary nebula (PN), A58. This event has long been ascribed to a final helium shell flash, but it has been suggested recently that it may instead have been an ONe nova. The new images provide an 18 yr baseline for the expansion of the ejecta from the 1919 event. In addition, the central star has been directly detected in the visible for the first time since 1923, when it faded from sight due to obscuration by dust. The expansion of the ejecta has a velocity of ∼200 km s-1, and an angular expansion rate of ∼10 mas yr-1, consistent with a 1919 ejection. This implies a geometric distance of 4.6 kpc for V605 Aql, consistent with previous estimates. The gas mass in the central knot of ejecta was previously estimated to be 5 × 10-5 M. It is estimated that warm dust associated with this gas has a mass of ∼10 -5 M. There is also evidence for a significant amount, 10 -3 M, of cold (75 K) dust, which may be associated with its PN. The knot ejected in 1919 is asymmetrical and is approximately aligned with the asymmetry of the surrounding PN. Polarimetric imaging was obtained to investigate whether the 2001 spectrum of V605 Aql was obtained primarily in scattered light from dust in the central knot, but the signal-to-noise in the data was insufficient to measure the level of polarization.
UR - http://www.scopus.com/inward/record.url?scp=84879994494&partnerID=8YFLogxK
U2 - 10.1088/0004-637X/771/2/130
DO - 10.1088/0004-637X/771/2/130
M3 - Article
AN - SCOPUS:84879994494
SN - 0004-637X
VL - 771
SP - 1
EP - 10
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 130
ER -