Abstract
We present Reflection Grating Spectrometer data from an XMM-Newton observation of the Seyfert 1 galaxy NGC 3516, taken while the continuum source was in an extremely low flux state. This observation offers a rare opportunity for a detailed study of emission from a Seyfert 1 galaxy, as these are usually dominated by high nuclear continuum levels and heavy absorption. The spectrum shows numerous narrow emission lines (FWHM ≲, 1300 km s-1) in the 0.3-2 keV range, including the H-like lines of C, N, and O and the He-like lines of N, O, and Ne. The emission-line ratios and the narrow width of the radiative recombination continuum of C VI indicate that the gas is photoionized and of fairly low temperature (kT ≲ 0.01 keV). The availability of emission lines from different elements for two isoelectronic sequences allows us to constrain the element abundances. These data show that the N lines are far stronger than would be expected from gas of solar abundances. Based on our photoionization models, we find that nitrogen is overabundant in the central regions of the galaxy, compared to carbon, oxygen, and neon, by at least a factor of 2.5. We suggest that this is the result of secondary production of nitrogen in intermediate-mass stars and indicative of the history of star formation in NGC 3516.
| Original language | English |
|---|---|
| Pages (from-to) | 128-135 |
| Number of pages | 8 |
| Journal | Astrophysical Journal |
| Volume | 594 |
| Issue number | 1 I |
| DOIs | |
| State | Published - Sep 1 2003 |
| Externally published | Yes |
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All Science Journal Classification (ASJC) codes
- Space and Planetary Science
- Nuclear and High Energy Physics
Cite this
Elemental abundances in NGC 3516. / Turner, T. J.; Kraemer, S. B.; Mushotzky, R. F.; George, I. M.; Gabel, Jack.
In: Astrophysical Journal, Vol. 594, No. 1 I, 01.09.2003, p. 128-135.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Elemental abundances in NGC 3516
AU - Turner, T. J.
AU - Kraemer, S. B.
AU - Mushotzky, R. F.
AU - George, I. M.
AU - Gabel, Jack
PY - 2003/9/1
Y1 - 2003/9/1
N2 - We present Reflection Grating Spectrometer data from an XMM-Newton observation of the Seyfert 1 galaxy NGC 3516, taken while the continuum source was in an extremely low flux state. This observation offers a rare opportunity for a detailed study of emission from a Seyfert 1 galaxy, as these are usually dominated by high nuclear continuum levels and heavy absorption. The spectrum shows numerous narrow emission lines (FWHM ≲, 1300 km s-1) in the 0.3-2 keV range, including the H-like lines of C, N, and O and the He-like lines of N, O, and Ne. The emission-line ratios and the narrow width of the radiative recombination continuum of C VI indicate that the gas is photoionized and of fairly low temperature (kT ≲ 0.01 keV). The availability of emission lines from different elements for two isoelectronic sequences allows us to constrain the element abundances. These data show that the N lines are far stronger than would be expected from gas of solar abundances. Based on our photoionization models, we find that nitrogen is overabundant in the central regions of the galaxy, compared to carbon, oxygen, and neon, by at least a factor of 2.5. We suggest that this is the result of secondary production of nitrogen in intermediate-mass stars and indicative of the history of star formation in NGC 3516.
AB - We present Reflection Grating Spectrometer data from an XMM-Newton observation of the Seyfert 1 galaxy NGC 3516, taken while the continuum source was in an extremely low flux state. This observation offers a rare opportunity for a detailed study of emission from a Seyfert 1 galaxy, as these are usually dominated by high nuclear continuum levels and heavy absorption. The spectrum shows numerous narrow emission lines (FWHM ≲, 1300 km s-1) in the 0.3-2 keV range, including the H-like lines of C, N, and O and the He-like lines of N, O, and Ne. The emission-line ratios and the narrow width of the radiative recombination continuum of C VI indicate that the gas is photoionized and of fairly low temperature (kT ≲ 0.01 keV). The availability of emission lines from different elements for two isoelectronic sequences allows us to constrain the element abundances. These data show that the N lines are far stronger than would be expected from gas of solar abundances. Based on our photoionization models, we find that nitrogen is overabundant in the central regions of the galaxy, compared to carbon, oxygen, and neon, by at least a factor of 2.5. We suggest that this is the result of secondary production of nitrogen in intermediate-mass stars and indicative of the history of star formation in NGC 3516.
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UR - http://www.scopus.com/inward/citedby.url?scp=0141457629&partnerID=8YFLogxK
U2 - 10.1086/376901
DO - 10.1086/376901
M3 - Article
AN - SCOPUS:0141457629
VL - 594
SP - 128
EP - 135
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1 I
ER -