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  • NOT/LAT monitoring

    Abstract

    NOT LAT monitoring

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    Introduction

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    Should be observed

    PKS 0507+17
    photometry and spectroscopy

    Results

    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

    Unid0143-5844

    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.
    Photometry:
    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    NOMAD B=17.63 V=17.74 YB6 Catalog (USNO, unpublished)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

    Unid0523-2530

    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.

    Next(??)::
    Estimate radio-optical-Xray spectral indices (or flux ratios)
    Data:
    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

    UNid0746-0222


    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
    Spectroscopy:
    2014-09-30 new grism 2200

    UNid0803-0339

    Next:
    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 s