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Optical to Far-IR Observations of 3C 446

Published online by Cambridge University Press:  05 March 2013

K.J. Leech ,
R. Saxton ,
P. Barr ,
M. Santos-Lleo ,
E. Jiminez-Bailon ,
R. Diaz ,
K. Ghosh  and
S. Soundararajaperumal
K.J. Leech
Affiliation:
ISO Data Centre, Astrophysics Division, ESA Space Science Department, P.O. Box 50727, 28080 Madrid, Spain; Kieron.Leech@said-business-school.oxford.ac.uk
R. Saxton
Affiliation:
Vega/ESA, XMM-SOC, University of Leicester, University Road, Leicester LE1 7RH, UK; rds@star.le.ac.uk
P. Barr
Affiliation:
Astrophysics Division, ESA Space Science Department, ESTEC Postbus 299, 2200 AG – Noordwijk, The Netherlands; Paul.Barr@astro.estec.esa.nl
M. Santos-Lleo
Affiliation:
XMM Science Operations, Astrophysics Division, ESA Space Science Department, P.O. Box 50727, 28080 Madrid, Spain; msantos@xmm.vilspa.esa.es
E. Jiminez-Bailon
Affiliation:
Laeff, P.O. Box 50727, 28080 Madrid, Spain
R. Diaz
Affiliation:
Observatorio Astronomico de Cordoba/SeCyT, UNC, Argentina
K. Ghosh
Affiliation:
Indian Institute of Astrophysics, Bangalore, 560034, India
S. Soundararajaperumal
Affiliation:
Indian Institute of Astrophysics, Bangalore, 560034, India
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Abstract

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The OVV blazar 3C 446 was monitored over seven months in 1997 with ground based telescopes and instruments on ESA's Infrared Space Observatory (ISO). The aim was to try to detect variations in the IR and see if these were correlated with optical variations. The object varied in the optical and near-IR during this period, but did not vary in the far-IR. Despite being a factor of ten weaker than in 1983, the optical-IR SED exhibited the same slope. The new far-IR observations from ISO allow us to determine the location of the turnover in the spectrum, caused by synchrotron self-absorption. It occurs just longwards of 100 μm.

Keywords

BL Lacertae objects: individual (3C 446)infrared: galaxies

Information

Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 19 , Issue 1 , 2002 , pp. 152 - 154
Copyright
Copyright © Astronomical Society of Australia 2002

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