NOT/LAT monitoring


NOT LAT monitoring

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Should be observed

PKS 0507+17
photometry and spectroscopy


Add the individula targets under this section

Unidentified LAT sources

Optical and spectrosopic identification of LAT sources from Acero et al astro-ph 1310.6735.
The Acero source are :
J0143-5844, J0523-2530, J0803-0339, J1036-6722, J1129+3758, J1231-5112 and J1844+1548


NTT and GMOS spectra show no lines, featureless spectrum most likely BL Lac, as proposed by Massaro et al
Check S/N of the spectra and wavelenght coverage.
Acero et al:
three x-ray sources in LAT error ellipse, A2 and A3 are faint soft sources and A1 is the brightest, some variability (?), however the hardness rasio does not change, an possibly an AGN. All three sources were UV detected, A1 did not show variability in UV.
A1, A2, A3 were detected in radio, however A1 is the strongest radio source (Roopesh, are the A2 A3 radio detections real?). Petrov et al (2013) detected this (these?) in radio as well.
A1 is a blazar candidate as it has flat radio sepctrum SED like a blazar SED and based on Massaro et al (2013) WISE data this is a BL Lac candidate.

This source is WISE detected.
Little variability based on three (GSC2.3, USNO-A2, USNO-B1) sky surveys. Typical B\(\sim\) 17.7 , (however USNO-B1 B2=18.48), R\(\sim\)16.7-17.0. The most recent estimate from our own GMOS data (r-filter) is about 16.6.

Archival data:
GSC2.3 J=17.71 F=16.98 N=16.73
NOMAD B=17.63 V=17.74 YB6 Catalog (USNO, unpublished)
2MASS J=15.817 H=15.021 K=14.269
USNO-A2 B=17.7 R=16.9
USNO-B1 B2=18.48 R1=16.70 R2=16.64 I=17.04


Acreo et al found only a dim X-ray source on the 2FGL field and non-detection in UV. In radio the X-ray counter part was detected only in the lowest radio frequency. \(\gamma\), X-ray, radio data might suggest a pulsar origin. EF \(i > \)21.8mag (9-11-2013)
Calibrated photometry:
No optical identification for 05:23:17.11 -25:27:31.9 source, indicating \(i>\)21.6mag. This source (05:23:17.11 -25:27:31.9) is not WISE detected.
The second candidate :
S21R009171 05 23 24.414 -05 23 24.414 (2000) J(GSC)=22.52+-0.71
wk07 i=19.54 +- 0.04
xj12 i=19.62 +- 0.08
xj13 B= 22.0+-0.12; V=21.66+-0.12; R=20.50+-0.06; i=19.72+- 0.06
xj21 R=20.61 +- 0.11
The optical colours are not similar to the Landolt std-stars or the field stars nor the Fukugita et al PASP 107 (1995) synthetic galaxy colours.
No significant variability based on the optical data.

Estimate radio-optical-Xray spectral indices (or flux ratios)
XX 08-11-2013 i 120+300+300 ALwk070141,4,5 thin clouds?
\(i >\) 21.8 mag (6.1 arcsec NE from a star)
XX14-01-2014 i 6x60sec ALxa140100 clouds non-detection
01-10-2014 z 8x120 ALxi300204-11
XX12-10-2014 i 2x90,B 120 ALxj120415-7 clouds
XX13-10-2014 BVRi 120,90,90,90 ALxj130989-993
XX21-10-2014 R 90,180 ALxj210209,10


The given position (07:46:05.52 -02:22:08.4) has two canidates for the optical countrparts: 3.3 arcsec East (c1) and 2.7 arcsec NW (c2) from the above coordinates (uncomoftably far away). Both of these have GSC2.3 magnitudes F=20.17 and 20.64, respectively.
Optical multiband (ugri) data suggest that the synchroton peak is in the NIR/IR region.
This source is WISE detected.
The archival data for c1 is:
GSC J=21.41 F=20.17 N=18.78
USNO-B1 B2=18.75 R2=19.60
c2 (only one detection):
GSC F=20.64
NOT photometry:
wa20 R-band: c1=19.8 c2=21.0
xa14 R-band: c1=19.7 (through thick clouds)
xc19 R-band: c1=19.8 c2=20.9
xa14 i-band: c1=18.9 (through thick clouds)
2013-01-21T01:55 R 60 ALwa200129
2014-01-14 R,i attempt, ALxa140170 thick clouds
2014-04-02 RVugriz twilight
2014-09-30 R 90 ALxi29+167
2014-09-30 new grism 2200


Based on ATCA does this object have flat or steep radio spectrum (Rooepsh??)?
Acero et al:
Only one X-ray source, two data point some variability in X-ray, not in UV. Broad band SED suggest AGN origin. Radio sepctrum evolved from flat to steep, howver non-simultaneous data (maybe indicates more like variability). The LAT data shos variability. Not detected by WISE.
Note: The NVSS radio source has coordinates 08 03 11.82 -03 35 58 this is 5.0arcsec NW from the star:
GSC2.3 S3MX011575 08 03 11.427 -08 03 11.427
and 6.9 arcsec SE from S3MX011575.
There are no optical identifications (\(R >\) 24.0 conservative limit) of the NVSS coordinates. This is based on preliminary analysis of 3x900sec r-band image (MOSCA april 2014). The \(Swift\) coordinates are 08:03:12.11 -03:36:01.4,
identified as GSC2.3 S3MX011550 08 03 12.090 -03 36 00.88 (F=17.73 J=18.66 N=17.55 B=19.27) USNO-A2 R=17.7 B=18.7 (1953) and USNO-B1 R1=17.5 R2=17.73 B1=19.10 B2=19.38 I=16.87
R:17.73, 17.5, 17.73 (no variability)
NOT R 18.55, 18.65, 18.68, 18.56, 18.28
B:18.7 18.7 19.10 19.38 (variable ?)
The \(Swift\) optical counterpart has a companion about 2.7 arcsec SE (R=20.3/20.4 ). Optical spectrum of the Swift target is extended and shows broad emission lines the companion has XXXX spectrum.
Spectroscopy quick look indicates redshift 0.37, lines e.g. 2x[OIII], [OII]H-be, MgII. Broad lines relatively weak EW aboput 5Åor less, however [OII] and [OIII] lines are strong EW about 15Åor more. The width of the broad lineas are between 1000 and 2000 km/s, suggesting NLSy1 spectral calssification.

This source is WISE detected.
Photometry, data:
Calibrated, final(?) photometry:
Calibration using GSC2.3 F and N magnitudes of the field stars.
2014-03-19T21:45:25.249 R=18.403 zero point std=0.09
2014-01-14T23:53:51.733 i=18.089 zero point stddev=0.064
2014-01-15T00:10 R=18.70 zero point stddev=0.12

Calibration using SDSS field with similar airmass:
2014-04-02T21:21:20.9 r = 18.38 (AB-mag)
zero point std: 0.014

  • s2: S3MX011526 ; s1:S3MX011575

  • UT tgt-s1 tgt-s2 s1-s2

  • 2013-06-02T20:56:31.840, 1.17 , 0.819, -0.351

  • 2013-09-23T05:56:42.950, 1.261, 0.912, -0.349

  • 2013-11-08T05:55:21.392, 1.148, 0.857, -0.291

  • 2014-01-15T00:10:37.290, 1.164, 0.866, -0.298

  • 2014-03-19T21:45:25.249, 1.149, 0.844, -0.305

  • 2014-04-02T21:21:20.9 , 0.922, 0.624, -0.298

Note the host galaxy will contribute to the tgt-magintudes.

XX 2013-06-02T20:46 R 30x3+90+180 ALwf020154
twlight R=18.55
XX 2013-09-23T05:55 R 180 ALwi220171
XX 2013-11-08T05:42 R 200,300x3 ALwk070173
XX 2014-01-14 i 3x50 secALxa140144 clouds
XX 2014-01-14 R 3x50 attempt,ALxa140150 thick clouds
XX 19-03-2014 R 60 ALxc190072
XX 2014-04-02 MOxd02 SDSS r 900
2014-04-03 MOxd03 SDSS 2x r 900
2013-11-08T05:18 gr4 1000 ALwk070169


Optical identification of this source is not clear.
The coordinates 08:38:51.36 -28:28:12.0 points 2.5 arcsec NNE from a R=19.7 target (s2). There is an indication that s2 is variable, as it is an EF in GSC2.3 and there are three faint features (F=19.76, 19.92 and F=19.94) withinn one arc min radius from the coordinates with R(wa20) 19.92, 19.92 and 19.95.

Optical multiband (BRi) data suggest that the synchroton peak is in the NIR/IR region.
This source is not WISE detected.
2013-01-21T02:00 R 60 ALwa200130
s2 R=19.7 2014-01-14 R,i attempt, ALxa140180 thick clouds
2014-04-03 MOxd03 BR


Do we have any NTT or GMOS data??
Acero et al:
Only two marginal X-ray sources, although extensively observed (35.5 ksec instead of the “normal” \(\sim\) 4 ksec). Marginal UV detection as well, not good enough detectyion for variability.
Radio detection only for D1 (5.5GHz), indicating steep radio spectrum and no WISE detection. This is a pulsar candidate.

This source is not WISE detected.
NTT R-band 200 sec EFOSC_Image365_0003


Next: take SDSS data (ugriz?) as this is an SDSS-field.

Acero et al:
This is a flatspectrum radio source with faint X-ray and UV-detections (Acero et al 2013). The radio-UV-X-ray data suggest that the syncrotron component has very low peak frequency, also this source might have high compton dominance (the ratio of peak Compton to the synchrotron luminosity). SDSS z=4.09 is highly speculative. Our own low resolution spectra show no lines (three epochs, however low S/N).

Based on three epochs of data Jan 14, Feb 3 and Feb 19 there is a clear indication of variability. The target got about 0.5 magnitudes (in R-band) and 0.3magnitudes (in i-band) fainter from January to February. This is using differential phtometry “tgt - comparison star” (5.69, 6.07, 6.16) vs “Comparison star - Check star” (-0.53, -0.54, -0.50).
in i-band the same epochs “tgt - comparison star” ( 5.66, 5.9 , 5.99) vs “Comparison star - Check star” (-0.58, -0.58, -0.57).

Optical multiband (ugriz) data suggest that the synchroton peak is in the NIR/IR region.
This source is WISE detected.
Spectroscopy 15-01-2014 g4 slit1.3 +WG345 1200 ALxa140214; no lines
04-02-2014 g4 slit1.3 +WG345 1200 ALxb030194
19-02-2014 g4 slit1.0 1500 ALxb190189 low S/N

Historical data:
GSC2.3 JFVN 19.90 19.25 18.45 18.82
SDSS ugriz 20.870, 20.256, 19.685, 19.334, 19.109
USNO A2 BR 19.1 18.7
USNO B1 B12,R12,N 19.90, 19.35; 19.23 19.48; 18.58
NOMAD V 17.97

15-01-2014 R,i 180,120 ALxa140205,6
04-02-2014 R,i 60,40 ALxb030185,6
19-02-2014 B,R,i 90,60,40 ALxb190179-31
frames are OK


Acero et al:
X-ray counts of this source are similar to the counts of 1129+3758E1 and both are also UV detected. this was not detected in radio (5.5 and 9GHz). In optical not yet detected, \(i >\)22.3 mag.

NOT ALFOSC ALxa14 (14-01-2014) 2x200+2x300 sec
Empty field i>22.3 mag
coadded image (frineg correction should be better) magnitudes measured using iraf/imexam six fai