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3C 286: a Bright, Compact, Stable, and Highly Polarized Calibrator For Astronomy & Astrophysics manuscript no. 3C286-pol-calib-v7.0 c ESO 2018 October 15, 2018 3C 286: a bright, compact, stable, and highly polarized calibrator for millimeter-wavelength observations Iv´an Agudo1,2, Clemens Thum3, Helmut Wiesemeyer4,5, Sol N. Molina1, Carolina Casadio1, Jos´eL. G´omez1, and Dimitrios Emmanoulopoulos6 1 Instituto de Astrof´ısica de Andaluc´ıa, CSIC, Apartado 3004, 18080, Granada, Spain e-mail: [email protected] 2 Institute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USA 3 Institut de Radio Astronomie Millim´etrique, 300 Rue de la Piscine, 38406 St. Martin d’H`eres, France 4 Max-Planck-Institut f¨ur Radioastronomie, Auf dem H¨ugel, 69, D-53121, Bonn, Germany 5 Instituto de Radio Astronom´ıa Milim´etrica, Avenida Divina Pastora, 7, Local 20, E–18012 Granada, Spain 6 School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK Preprint online version: October 15, 2018 ABSTRACT Context. A number of millimeter and submillimeter facilities with linear polarization observing capabilities have started operating during last years. These facilities, as well as other previous millimeter telescopes and interferometers, require bright and stable linear polarization calibrators to calibrate new instruments and to monitor their instrumental polarization. The current limited number of adequate calibrators implies difficulties in the acquisition of these calibration observations. Aims. Looking for additional linear polarization calibrators in the millimeter spectral range, in mid-2006 we started monitoring 3C 286, a standard and highly stable polarization calibrator for radio observations. Methods. Here we present the 3 and 1 mm monitoring observations obtained between September 2006 and January 2012 with the XPOL polarimeter on the IRAM 30 m Millimeter Telescope. Results. Our observations show that 3C 286 is a bright source of constant total flux with 3 mm flux density S 3mm = (0.91 ± 0.02) Jy. ◦ The 3 mm linear polarization degree (p3mm = [13.5 ± 0.3] %) and polarization angle (χ3mm = [37.3 ± 0.8] , expressed in the equatorial coordinate system) are also constant during the time span of our observations. Although with poorer time sampling and signal-to-noise ratio, our 1 mm observations of 3C 286 are also reproduced by a constant source of 1 mm flux density (S 1mm = [0.30 ± 0.03] Jy), ◦ polarization fraction (p1mm = [14.4 ± 1.8] %), and polarization angle (χ1mm = [33.1 ± 5.7] ). Conclusions. This, together with the previously known compact structure of 3C 286 –extended by ∼ 3.5′′ in the sky– allow us to propose 3C 286 as a new calibrator for both single dish and interferometric polarization observations at 3 mm, and possibly at shorter wavelengths. Key words. Polarization – Instrumentation: polarimeters – Techniques: polarimetric – Galaxies: quasars: individual: 3C 286 – Submillimeter: general – Radio continuum: general 1. Introduction calibrators (& 5′, where 5′ is the approximate angular exten- sion of the Crab nebula at millimeter wavelengths; Aumont et al. 2010) may make difficult polarization calibration observations arXiv:1201.2150v2 [astro-ph.IM] 29 Feb 2012 Despite the recent start of operations of a considerable num- at angular resolutions better than that. Even when this is not the ber of millimeter observing facilities with ability for high case, the poor coverage of adequate calibrators in the sky often precision polarization measurements (e.g., ALMA, PLANK, reveals the need for new polarized sources suitable for calibra- IRAM 30m Telescope and PdB Interferometer, SMA, KVN, tion. BOOMERANG, CBI, MAXIPOL, QUaD, WMAP, and BICEP), the number of suitable polarization calibrators is still limited. In this paper we present the results from series of millime- The most commonly used sources for calibration of millime- ter measurements with the IRAM 30m Telescope to character- h m ter polarization observations are the Crab nebula (Taurus A, ize 3C 286 (with J2000 equatorial coordinates: α = 13 31 s ◦ ′ ′′ Aumont et al. 2010), Centaurus A (Zemcov et al. 2010), the 8.3 , δ = +30 30 33 ) as a new bright, compact, stable, and limb of the Moon (Barvainis et al. 1988; Thum et al. 2003), and highly polarized calibrator for short millimeter observations. the diffuse Galactic emission (Matsumura et al. 2010). An ideal This source has been widely used for calibration at centime- linearly polarized calibrator is a point-like, bright and constant ter radio wavelengths both for total flux (Baars et al. 1977; Ott source of high linear-polarization fraction with well defined and et al. 1994; Kraus et al. 1999) and linear polarization observa- constant polarization angle. For most facilities designed to study tions (Perley 1982; McKinnon 1992; Taylor et al. 2001; G´omez the polarization properties of the cosmic microwave background, et al. 2002). which still do not aim at observations with angular resolutions 3C 286 is a bright compact steep spectrum radio quasar much better than ∼ 5′, one or more among the four calibrators (Peacock & Wall 1982; Fanti et al. 1985) at a redshift z = 0.849 mentioned above fulfill most of these conditions. However, the (Burbidge & Burbidge 1969). Radio imaging with the Very relatively large angular extension of all these four polarization Large Array at sub-arcsecond resolution has revealed an 1 Agudo et al.: 3C 286: a polarization calibrator for millimeter observations extended structure composed of three misaligned bright fea- Table 1. 3 mm photo-polarimetric data from 3C 286. tures (e.g., Akujor & Garrington 1995). Among these three ′′ structures, the second one in brightness is located 2.6 West– Date RJD S 3mm p3mm χ3mm South–West from the brightest one. Both of them are linked days Jy % ◦ by a nearly straight jet-like bridge of radio emission seen 2006-09-24 54003 0.92 ± 0.05 15.6 ± 0.5 39.0 ± 1.0 in high dynamic range images. The third emission region is 2006-10-03 54012 1.03 ± 0.05 13.4 ± 0.4 40.0 ± 1.1 located at 0.8′′ East from the brightest one. Among these 2006-10-13 54022 0.90 ± 0.05 12.2 ± 0.4 39.0 ± 1.6 three emission features, the two brightest ones dominate the 2006-10-14 54023 0.94 ± 0.05 14.4 ± 2.1 40.0 ± 2.6 linear polarization emission, and show their electric vector 2006-11-16 54056 0.87 ± 0.04 12.8 ± 1.1 32.1 ± 1.9 oriented nearly parallel to the axis of the jet like structure 2006-11-17 54057 0.85 ± 0.04 16.6 ± 0.6 39.5 ± 0.9 between them. The integrated electric vector polarization 2006-11-22 54062 0.90 ± 0.04 13.9 ± 0.5 41.8 ± 2.2 angle of the source1 χ ≈ 33◦ at all observing wavelengths 2006-12-01 54071 0.92 ± 0.05 14.1 ± 0.8 37.1 ± 1.1 ± ± ± from 20cm to 7mm (Perley 1982; Taylor et al. 2001), see 2007-01-03 54104 0.96 0.05 14.0 1.4 38.4 1.5 2007-01-17 54119 0.97 ± 0.05 14.9 ± 0.4 41.9 ± 1.0 also http://www.vla.nrao.edu/astro/calib/polar/. 2007-01-29 54130 0.94 ± 0.05 13.4 ± 0.4 36.1 ± 1.0 The stability of χ along radio frequencies has also been 2007-06-11 54262 0.83 ± 0.04 14.8 ± 0.7 31.1 ± 1.3 demonstrated through polarization angle rotation measure 2007-08-07 54320 1.00 ± 0.05 ... ... studies (Rudnick & Jones 1983). Very long baseline inter- 2007-10-09 54383 0.85 ± 0.04 15.6 ± 0.4 37.4 ± 1.0 ferometric radio observations at milliarcsecond resolution 2008-05-04 54591 0.87 ± 0.06 13.3 ± 0.8 30.1 ± 1.9 of the brighter, and more compact, feature have revealed a 2008-05-13 54600 0.95 ± 0.05 ... ... well defined jet structure initially oriented in the South–West 2008-12-29 54830 1.02 ± 0.05 13.5 ± 0.4 39.1 ± 1.1 direction up to scales > 60 milliarcseconds, with the linear 2009-06-18 55001 0.87 ± 0.04 13.0 ± 0.3 39.4 ± 0.8 polarization fraction ranging from p ≈ 1% and p ≈ 20 % 2009-07-30 55043 0.90 ± 0.04 14.9 ± 1.1 38.9 ± 1.3 ± ± ± and χ oriented nearly (but not exactly) parallel to the local jet 2009-08-18 55062 0.90 0.04 13.9 0.4 36.6 2.1 2010-05-05 55322 0.98 ± 0.05 13.6 ± 0.4 37.5 ± 2.4 axis (Jiang et al. 1996). These properties are not uncommon 2010-06-06 55354 0.94 ± 0.05 12.6 ± 0.3 37.3 ± 1.1 in radio loud quasar jets. However, 3C 286 lacks a highly 2010-06-16 55364 0.83 ± 0.04 13.5 ± 0.3 37.5 ± 0.7 variable, low polarization, and high brightness temperature 2010-08-15 55424 0.83 ± 0.04 15.4 ± 0.3 38.4 ± 0.7 10 11 (Tb & 10 –10 K) radio core (Cotton et al. 1997), as typical 2010-10-12 55482 0.93 ± 0.05 13.0 ± 0.3 33.8 ± 0.8 for radio quasars. This makes 3C 286 an excellent total flux 2011-01-31 55593 0.87 ± 0.04 13.4 ± 0.3 33.0 ± 0.7 and polarization calibrator at radio wavelengths, and provides 2011-02-07 55600 0.95 ± 0.05 13.5 ± 0.3 35.2 ± 0.7 it with its characteristic non variable, and large integrated 2011-03-25 55646 0.94 ± 0.05 13.5 ± 0.2 38.5 ± 0.7 linear polarization degree (p ≈ 11%) at radio frequencies 2011-04-10 55662 0.92 ± 0.05 13.4 ± 0.3 37.6 ± 0.7 (http://www.vla.nrao.edu/astro/calib/polar/).
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