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The Acero source are :\\  J0143-5844, J0523-2530, J0803-0339, J1036-6722, J1129+3758, J1231-5112 and J1844+1548  \subsection{Unid0143-5844} Do we have NTT or GMOS data?\\  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.     \subsection{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)\\   Next:\\  Estimate radio-optical-Xray spectral indices (or flux ratios)\\    Data:\\   08-11-2013 i 120+300+300 ALwk070141,4,5 thin clouds?\\   $i >$ 21.8 mag (6.1 arcsec NE from a star)\\   14-01-2014 i 6x60sec ALxa140100 clouds\\    \subsection{UNidJ1844+1546}   \textbf{Photometry}\\   2013-07-18T21:54 R 90 ALwg180095\\   \subsection{UNid0746-0222}\\   2013-01-21T01:55 R 60 ALwa200129\\  2014-01-14 R,i attempt, ALxa140170 thick clouds\\     \textbf{Spectroscopy:}\\   2013-07-18T22:04 gr4 600 ALwg180099\\     \subsection{UNid0803-0339}     Next: \\   Deep image to confirm the NVSS optical id\\   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 6.6arcsec SE from the star:\\   GSC2.3 S3MX011575 08 03 11.427 -08 03 11.427 \\   and there are no clear optical identifications ($R >$ 23.5 (conservative limit), however some fint excess   near the expected radio location $R \sim$ 25.4mag (????) ).   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\\   B:18.7 18.7 19.10 19.38 (variable ?)\\   The $Swift$ optical counter part has a companion about 2.7 arcse SE (R=20.3/20.4 ).  Optical spectrum of the Swift target is extended and shows broad emission lines   the companion has XXXX spectrum.     \textbf{Photometry, data:}\\   \textbf{Photometry} 2013-06-02T20:46 R 30x3+90+180 ALwf020154\\   twlight R=18.55\\  2013-09-23T05:55 R 180 ALwi220171\\  R=18.65\\   2013-11-08T05:42 R 200,300x3 ALwk070173\\   R=18.68\\   2014-01-14 i 3x50 secALxa140144 clouds\\  2014-01-14 R 3x50 attempt,ALxa140150 thick clouds\\  19-03-2014 R 60 ALxc190072\\   R=18.56\\  \textbf{Spectroscopy:}\\   2013-11-08T05:18 gr4 1000 ALwk070169\\   \subsection{UNid0746-0222}\\   2013-01-21T01:55 R 60 ALwa200129\\     \subsection{UNid0838-2828}\\  2013-01-21T02:00 R 60 ALwa200130\\   2014-01-14 R,i attempt, ALxa140180 thick clouds\\     \subsection{UNid1036-6722}     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.     \subsection{1129+3758E1}     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).    \textbf{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\\  \textbf{Photometry}    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     \subsection{1129+3758E2}     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 faint field stars zp(correction)std=0.06\\    faintest features are about i-mag=22.3     \subsection{UNid1221-0633}\\    2013-01-21T06:29 R 60 ALwa200169\\  2014-02-20T04:05 R 2x300 ALxb190177,8\\   single frame EF\\  2013-03-11 i 3x400 reduced & combined data i(Vega) about 23.1\\  Next:\\   1)find the nearly simultaneous SDSS gri colours\\   2) get radio flux (and X-ray ?) to get the spectral indices (radio-optial-Xray)\\      \subsection{UNid1231-5112} Do we have any NTT or GMOS data?\\    Acero et al:\\  Three X-ray sources are detected in the error ellipse (F1,F2,F3).\\   F1 is a hard source, while F2 and F3 are soft. F1 and F2 have   dim optical counter part and F3 is a bright star.   This is the only $\gamma$ ray source (of the Acero sample) which had no radio  source with an upper limit of 10mJy at 5.5 and 9 GHz. The LAT proerties are not quite as for a typical pulsar,   however the multi wavelenght proerties are not like AGN either.    \subsection{UNidJ1844+1546}     Next:\\   1)measure optical linear polarization (compare synchrotron peak vs polarization)\\   2)find the nearly simultaneous SDSS gri colours (to comare this to known SDSS sources)\\   3) get radio flux (and X-ray ?) to get the spectral indices (radio-optial-Xray)\\     Acero et al (2013) reported variability in X-rays (factor of five or about 1.7 magnitudes) and in  UV($Swift$ M2 filter) one magnitude, however in optical the varaibility might be more modest.  Historical data suggest some variability e.g. B: 18.65, 18.6, 18.90, 18.45, 18.25   and 19.27 R: 17.22, 17.7 18.17, 17.15, 17.97 but nothing dramatic, especially taking into account the  measurement errors 0.3-0.4 mag.    Our own data from 07-2013 and 03-2014 show again some variability $\Delta R \sim$ 0.33 mag,  where the error estimate is $<<$ 0.1     \subsection{1129+3758E2}   NOT ALFOSC ALxa14 (14-01-2014) 2x200+2x300 sec \\   Empty field i>22.3 mag (of the difference).  In optical (R-band) the target is unresolved (FWHM $\sim$ 1 arcsec), however the  images are not deep, ruling out only very low redshifts ($\le$0.05) assuming that the   object is a typical blazar.   Our optical lowresolution spectroscopy suggest that the target is a BL Lac object.   The first spectrum (07-2013) has rather low S/N (about XX at best), but show just   a featureless continuum. The second spectrum (03-2014) has higher S/N but still no   lines, suggesting that the traget is BL Lac object rather than NLSy1, suggested by Acero et al (2013).   The BL Lac identification agrees with the infrared colour classification by Massaro et al. (2013).   Preliminary optical polarization supports the BL Lac identification.   The measured linear polarization (needs to \\   coadded image (frineg correction should be confirmed) is similar what to expect from  low energy peaked BL Lacs (classically radio selected BL Lacs).  \textbf{Photometry}\\   Background:\\   there is a star 2.8" W from the tgt R better) magnitudes measured using iraf/imexam   six faint field stars zp(correction)std=0.06\\   faintest features are about 19.9mag\\  Historical data:\\   GSC2.3 JFVN 18.65 17.22 17.96 16.40 (1993.379?) B(POSS-I) 19.27\\  USNO A2 BR 18.6 17.7 1951.528\\  USNO B1 B1,B2,R1,R2,I 18.90, 18.45, 18.17, 17.15, 16.00 \\  NOMAD BV 18.35, 17.97 YB6 catalogue, unpublished)\\  Our own data:\\   2013-07-18T21:54 R 90 ALwg180095\\    R=17.47 (quick look assuming R=F)\\   2014-03-11 R 90 ALxc110446\\  R=17.16 (quick look assuming R=F)\\  2014-03-19 R 60 sec ALxc190220\\  R=17.19 (quick look assuming R=F)\\   tgt-s2 0.15(wg18) -.18(xc11) -.13(xc18)\\  tgt-s5 0.18(wg18) -.12(xc11) -.06(xc18)\\   s2-s5 .03(wg18) .06(xc11) .07(xc18)\\    \textbf{Optical polarization:}\\   2014-03-19 R 4x90 sec ALxc190227-30\\   quick look P$\sim$9\%   \textbf{Spectroscopy:}\\   2013-07-18T22:04 gr4 600 ALwg180099\\   2013-03-11 gr4 1200 ALxc110453 no lines S/N up to 60\\  i-mag=22.3  \subsection{UNidJ1844+1546}  \textbf{Photometry}\\  2013-07-18T21:54 R 90 ALwg180095\\