1FGL AGNs at parsec scales (south)


Introduction

We observed with the LBA 46 counterparts from the 1FGL catalogue of γ-ray sources discovered by Fermi with delcinations < -30° which were not studied before at parsec scales. Their total flux densities at 8 GHz as found by Abdo et al. (2010b) and by our analysis to be in the range of about 1 to 100 mJy. Despite the previous view that γ-ray detected AGN are identified with extragalactic objects showing flat radio spectra — an indicator of a compact boosted relativistic jet — some of these objects show peaked or even steep radio spectra. We will extend analysis of AGNs detected by the Fermi LAT and correlate properties of AGN γ-ray emission with properties of parsec-scale radio emission. We assume that the AGN -ray emission is generated in the regions close to the central super-massive black hole, therefore are interested to compare it with the radio emission from nearby regions. We eliminate the current VLBI sample bias towards strong radio jets in order to draw meaningful conclusions from our analysis.

Scientific goal

On the basis of our previous analysis (e.g., Kovalev et al. 2009), we do expect to detect significant parsec-scale emission for most of the targets. In the same time, the cases of non-detections will provide a very important basis to test SED models of emission. This project will deliver the following observational results:

People

Team members (in alphabetic order):

Source list

The list of 46 observed sources.

Current status

Preliminary results

Experiment v441a
Experiment v441a (FAPSO)

Schedule

Data

Correlator output in FITS-IDI format (145.7 Gb):

2011_11_12_v441a_01.fits
2011_11_12_v441a_02.fits
2011_11_12_v441a_03.fits
2011_11_12_v441a_04.fits
2011_11_12_v441a_05.fits
2011_11_12_v441a_06.fits
2011_11_12_v441a_07.fits
2011_11_12_v441a_08.fits
2011_11_12_v441a_09.fits
2011_11_12_v441a_10.fits
2011_11_12_v441a_11.fits
2011_11_12_v441a_12.fits
2011_11_12_v441a_13.fits
2011_11_12_v441a_14.fits
2011_11_12_v441a_15.fits

Calibration

Station Log Weather Tsys
ATCA-104 n/a v441a_at.ant v441a_at.ant (Constant 50K)
CEDUNA v441acd.log v441acd.log v441a_cd.ant
DSS34 n/a n/a v441a_ti.ant
HARTRAO v441ahh.log v441ahh.log v441a_hh.ant
HOBART26 v441aho.log v441aho.log v441a_ho.ant
MOPRA n/a v441a_mp.ant v441a_mp.ant
PARKES n/a v441a_pa.ant v441a_pa.ant

Comments

Results

36 out of 46 target sources had 3 or more used points. 10 non-detections:

0415-441
0451-282
0553-437
1205-508
1536-465
1638-530
1645-302
1930-812
2126-544
2352-531

System equivalent flux density (SEFD)

Station SEFD   Jy m.e.f.(SEFD) Opacity
ATCA-104 150 0.07 0.01
CEDUNA 1100 0.07 0.01
DSS34 260 0.25 0.01
HOBART26 910 0.07 0.00
MOPRA 530 0.08 0.02
PARKES 260 0.09 0.01

Estimates of the correlated flux density

The correlated flux density is given in three ranges:

Flux1:   0 – 6 Mλ
Flux2:   6 – 25 Mλ
Flux3:   25 – 50 Mλ

Source J2000 name # Obs Flux1   Jy Flux2   Jy Flux3   Jy
0010-401 J0012-3954 20 0.600 0.609 0.495
0017-569 J0019-5641 24 0.184 0.187 0.154
0017-821 J0019-8152 25 0.027 0.036 0.034
0020-521 J0022-5153 24 0.126 0.112 0.073
0156-397 J0158-3933 24 0.082 0.065 0.065
0215-668 J0216-6636 19 0.039 0.036 0.030
0235-362 J0237-3603 5 0.021 0.021 0.017
0235-618 J0236-6136 3 0.480 0.278 -1.000
0236-393 J0238-3905 22 0.044 0.046 0.036
0314-647 J0315-6436 6 0.027 0.017 0.020
0324-566 J0325-5629 16 0.050 -1.000 0.045
0324-567 J0325-5635 11 0.028 0.027 0.029
0438-436 J0440-4333 10 1.267 0.754 0.559
0447-439 J0449-4350 27 0.130 0.152 0.098
0517-726 J0516-7237 3 -1.000 0.359 0.363
0647-609 J0647-6058 23 0.050 0.063 0.054
0704-487 J0705-4847 11 0.022 0.011 0.015
0717-432 J0718-4319 18 0.039 0.037 0.035
0719-499 J0720-5004 20 0.071 0.028 0.060
0722+145 J0725+1425 3 -1.000 -1.000 0.745
0730-659 J0730-6602 17 0.041 0.030 0.048
1006-314 J1008-3139 16 0.058 0.041 0.048
1057-797 J1058-8003 11 4.120 3.997 4.312
1104-365 J1106-3646 16 0.099 0.063 0.083
1115-483 J1117-4838 16 0.111 0.074 0.104
1129-580 J1131-5818 10 1.366 0.744 1.426
1149-084 J1152-0841 8 0.692 0.119 0.691
1304-427 J1307-4259 17 0.032 0.022 0.032
1327+321 J1329+3154 3 -1.000 0.818 0.481
1341-337 J1344-3359 7 0.037 0.016 0.025
1414-435 J1417-4349 23 0.056 0.031 0.067
1424-418 J1427-4206 20 1.971 2.516 2.090
1442-469 J1446-4709 19 0.047 0.034 0.047
1530-798 J1537-7958 18 0.081 0.078 0.071
1605-666 J1610-6649 27 0.044 0.040 0.035
1619-765 J1626-7638 29 0.066 0.048 0.058
1655-532 J1659-5320 17 0.030 0.039 0.028
1656-075 J1658-0739 3 -1.000 0.406 0.308
1755-483 J1758-4821 30 0.324 0.322 0.297
1809-642 J1814-6412 16 0.072 0.081 0.054
1831-711 J1837-7108 8 0.678 1.011 0.870
1845-432 J1849-4314 18 0.220 0.072 0.227
1920-211 J1923-2104 3 -1.000 1.745 1.063
1933-474 J1936-4719 23 0.027 0.026 0.024
1935-692 J1940-6907 9 0.842 0.620 0.490
2059-627 J2103-6232 22 0.080 0.040 0.064
2109-484 J2112-4817 14 0.030 0.029 0.028
2128-545 J2132-5420 25 0.212 0.237 0.182
2136-428 J2139-4235 20 0.136 0.148 0.116
2142-758 J2147-7536 10 1.405 1.893 1.274
2215+020 J2217+0220 3 -1.000 -1.000 0.128
2232-488 J2235-4835 9 1.178 0.706 1.099
2247-423 J2250-4206 14 0.085 0.042 0.066
2252-830 J2257-8246 15 0.031 0.027 0.023

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This page was prepared by Leonid Petrov ()
Last update: 2013.01.28_08:03:46

Back to astronomy projects

This web page was prepared by Leonid Petrov ()
Last update: 2014.08.02_16:33:49