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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
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: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 13 53 03.5 +69 18 29 Mkn 279 = QSO 1351+695 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
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
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
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
Note (1): Instrumental magnitudes, not scaled to any standard system
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 9 F9.1 d HJD Heliocentric Julian Date 11- 14 F4.2 10-17W/m2/nm F5100A Optical continuum (at 5100AA) (1) 16- 19 F4.2 10-17W/m2/nm e_F5100A rms uncertainty on F5100A 21- 24 F4.2 10-16W/m2 FHb Hbeta flux (1) 26- 29 F4.2 10-16W/m2 e_FHb rms uncertainty on Hb
Note (1): F5100A is expressed in 10-15ergs/s/cm2/Å FHb is expressed in 10-13ergs/s/cm2
Acknowledgements: Maria Santos-Lleo
(End) Patricia Bauer [CDS] 06-Feb-2001
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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