TY - JOUR
T1 - Ionized gas and planetary nebulae in the bulge of the blue S0 galaxy NGC 5102
AU - McMillan, Russet
AU - Ciardullo, Robin
AU - Jacoby, George H.
N1 - Copyright:
Copyright 2020 Elsevier B.V., All rights reserved.
PY - 1994/11
Y1 - 1994/11
N2 - We present the results of an investigation into the morphology and dynamics of ionized gas in the bulge of the gas-rich S0 galaxy NGC 5102. We show that the bulge of NGC 5102 contains a ring of ionized gas, ∼1.3 kpc in diameter, which is centered well away from the nucleus. Through spectroscopy and [O III] λ5007 imaging, we show that the gas is excited by a low-velocity shock, which varies from ∼50 to ∼70 km s-1 along the ring. Fabry-Perot images in Hα confirm that the gas is moving slowly, and suggest that the structure is a supershell, ∼107 yr old. This age is significantly younger than the galaxy's nuclear starburst, which is ∼2×108 yr old. We also use our [O III] λ5007 images to identify planetary nebulae (PNs) in the bulge and inner disk of NGC 5102. Using the planetary nebula luminosity function, we derive a distance modulus to the galaxy of (m-M)0=27.47+0.18-0.27, or 3.1+0.3-0.4 Mpc, confirming its membership in the NGC 5128 group. Our derived value of 47.2+12.2-9.2×10-9 for the bolometric luminosity-specific PN density, α2.5, is higher than that observed for the bulge of M31 or the giant ellipticals of the Virgo Cluster, but not significantly different from that found for the small, normal ellipticals NGC 3377 or M32. The high value for α2.5 suggests that virtually all of NGC 5102's stars will someday evolve through the planetary nebula stage.
AB - We present the results of an investigation into the morphology and dynamics of ionized gas in the bulge of the gas-rich S0 galaxy NGC 5102. We show that the bulge of NGC 5102 contains a ring of ionized gas, ∼1.3 kpc in diameter, which is centered well away from the nucleus. Through spectroscopy and [O III] λ5007 imaging, we show that the gas is excited by a low-velocity shock, which varies from ∼50 to ∼70 km s-1 along the ring. Fabry-Perot images in Hα confirm that the gas is moving slowly, and suggest that the structure is a supershell, ∼107 yr old. This age is significantly younger than the galaxy's nuclear starburst, which is ∼2×108 yr old. We also use our [O III] λ5007 images to identify planetary nebulae (PNs) in the bulge and inner disk of NGC 5102. Using the planetary nebula luminosity function, we derive a distance modulus to the galaxy of (m-M)0=27.47+0.18-0.27, or 3.1+0.3-0.4 Mpc, confirming its membership in the NGC 5128 group. Our derived value of 47.2+12.2-9.2×10-9 for the bolometric luminosity-specific PN density, α2.5, is higher than that observed for the bulge of M31 or the giant ellipticals of the Virgo Cluster, but not significantly different from that found for the small, normal ellipticals NGC 3377 or M32. The high value for α2.5 suggests that virtually all of NGC 5102's stars will someday evolve through the planetary nebula stage.
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U2 - 10.1086/117181
DO - 10.1086/117181
M3 - Article
AN - SCOPUS:0042808633
SN - 0004-6256
VL - 108
SP - 1610
EP - 1618
JO - Astronomical Journal
JF - Astronomical Journal
IS - 5
ER -