J/A+A/369/57 Monitoring Mkn 279 in BVRI and Hβ fluxes (Santos-Lleo+, 2001)
Monitoring of the optical and 2.5-11.7 micrometer spectrum and mid-IR imaging
of the Seyfert 1 galaxy Mkn 279 with ISO.
Santos-Lleo M., Clavel J., Schulz B., Altieri B., Barr P., Alloin D.
Berlind P., Bertram R., Crenshaw D, Edelson R.A., Giveon U., Horne K.,
Huchra J.P., Kaspi S., Kriss G.A., Krolik J.H., Malkan M.A., Malkov Yu.F.,
Netzer H., O'Brien P.T., Peterson B.M., Pogge R.W., Pronik V.I., Qian B.-C.,
Reichert G.A., Rodriguez-Pascual P.M., Sergeev S.G., Tao J., Tokarz S.,
Wagner R.M., Wamsteker W., Wilkes B.J.
<Astron. Astrophys. 369, 57 (2001)>
=2001A&A...369...57S 2001A&A...369...57S
ADC_Keywords: Galaxies, Seyfert ; Photometry, UBVRI ; Spectroscopy
Keywords: galaxies: active - galaxies: individual: Mrk 279 - galaxies: nuclei -
galaxies: Seyfert - infrared: galaxies
Abstract:
Mid-infrared images of the Seyfert 1 galaxy Mrk 279 obtained with the
ISO satellite are presented together with the results of a one-year
monitoring campaign of the 2.5-11.7µm spectrum. Contemporaneous
optical photometric and spectrophotometric observations are also
presented. The galaxy appears as a point-like source at the resolution
of the ISOCAM instrument (4-5"). The 2.5-11.7µm average spectrum of
the nucleus in Mrk 279 shows a strong power law continuum with
α=-0.80±0.05 (Fν∝να) and weak PAH
emission features. The Mrk 279 spectral energy distribution shows a
mid-IR bump, which extends from 2 to 15-20µm. The mid-IR bump is
consistent with thermal emission from dust grains at a distance of
>100 light-days. No significant variations of the mid-IR flux have been
detected during our observing campaign, consistent with the relatively
low amplitude (∼10% rms) of the optical variability during the
campaign. The time delay for Hβ line emission in response to the
optical continuum variations is τ=16.7+5.3-5.6days, consistent
with previous measurements.
Objects:
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RA (2000) DE Designation(s)
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13 53 03.5 +69 18 29 Mkn 279 = QSO 1351+695
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 72 17 Optical Photometry from Wise Observatory
table5.dat 29 121 Optical Continuum and Hβ fluxes
tables.tex 74 302 LaTeX version of the tables
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 10 A10 "YYYY/MM/DD" Date UT Date
12- 20 F9.1 d HJD Heliocentric Julian Date
22- 27 F6.3 mag Bmag B magnitude (1)
29- 33 F5.3 mag e_Bmag rms uncertainty on Bmag
35- 40 F6.3 mag Vmag ? V magnitude (1)
42- 46 F5.3 mag e_Vmag ? rms uncertainty on Vmag
48- 53 F6.3 mag Rmag R magnitude (1)
55- 59 F5.3 mag e_Rmag rms uncertainty on Rmag
61- 66 F6.3 mag Imag ? I magnitude (1)
68- 72 F5.3 mag e_Imag ? rms uncertainty on Imag
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Note (1): Instrumental magnitudes, not scaled to any standard system
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 9 F9.1 d HJD Heliocentric Julian Date
11- 14 F4.2 10-17W/m2/nm F5100A Optical continuum (at 5100Å) (1)
16- 19 F4.2 10-17W/m2/nm e_F5100A rms uncertainty on F5100A
21- 24 F4.2 10-16W/m2 FHb Hβ flux (1)
26- 29 F4.2 10-16W/m2 e_FHb rms uncertainty on Hb
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Note (1): F5100A is expressed in 10-15ergs/s/cm2/Å
FHb is expressed in 10-13ergs/s/cm2
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Acknowledgements: Maria Santos-Lleo
(End) Patricia Bauer [CDS] 06-Feb-2001