Graphs

OJ 287

OJ 287

This is one of the most extensively studied blazars. Photographic observations extend back into the late 1800s (though
note how sparse the coverage is before about 1970). Superimposed on slow undulating variations lasting several decades, there are rapid outbursts of 4 magnitudes or more. There is some weak indication of periodicity for the outbursts, with an 11 year cycle. The outbursts themselves often appear double. It has been suggested that the central supermassive blackhole driving the activity may be a binary. Takalo and Sillanpaa (1999)

B2 1308+326

B2 1308+326

The B light curve for B2 1308+326 with respect to the modified JD. This source seems to exhibit primarily short-term outbursts. Fan and Lin (2000)

PG 1626+554

PG 1626+554

The R (filled) and B (open) lightcurves for PG 1626+554 over a period of approximately 7 years. The horizontal axis is in days. This source does not seem to exhibit violent outbursts or declines. It exhibited a modest but steady rise throughout this interval. Giveon et al. (1999)

AO 0235+164

AO 0235+164

The B light curve for AO 0235+164 in terms of the modified JD. This is an extensively studied object which exhibits short-term outbursts and declines. Fan and Lin (2000)

PG 0804+762

PG 0804+762

The R (filled) and B (open) lightcurves for PG 0804+762 over a period of approximately 7 years. The horizontal axis is in days. This source does not seem to exhibit violent outbursts or declines, but merely slow, irregular variations. Giveon et al. (1999)

PG 1704+608

PG 1704+608

The R (filled) and B (open) lightcurves for PG 1704+608 over a period of approximately 7 years. The horizontal axis is in
days. This source does not seem to exhibit violent outbursts or declines. It exhibited only a modest decline over this interval… except for the last observation which seems to indicate that an outburst had taken place. Giveon et al. (1999)

B2 1215+303

B2 1215+303

The B light curve for B2 1215+303 with respect to the modified JD. This object appears to be mostly in a “high” state that is occasionally interrupted by episodes of generally lower activity. Fan and Lin (2000)

PG 1001+054

PG 1001+054

The R (filled) and B (open) lightcurves for PG 1001+054 over a period of approximately 7 years. The horizontal axis is in
days. This source does not seem to exhibit violent outbursts or declines. The general trend is a slow decline, interrupted by a modest outburst lasting approximately 600 days. Giveon et al. (1999)

PKS 0754+100

PKS 0754+100

The B light curve for PKS 0754+100 with respect to the modified JD. This source exhibits moderate, irregular fluctuations of about 1 magnitude that seem to last less than a year. Occasional large, longer declines can approach 2 magnitudes. Fan and Lin (2000)

BL Lac

BL Lac

The V light curve for BL Lac over a period of about 1 year. In addition to the slow irregular variation of 2 magnitudes over this period, irregular outbursts and declines of more than 1 magnitude can be seen to occur over periods of several days. Tosti et al. (1999)

PKS 0735+178

PKS 0735+178

The R lightcurve fpr PKS 0735+178 over a period of about 6 years. During periods of coverage, significant variation of nearly 2 magnitudes can be seen over periods of several months. Significant variations over several days are clearly evident in the data. Tosti et al. (1999)

Mark 421

Mark 421

The magnitude variation (unspecified band) for Mrk 421 on 13 March 1981. The x-axis is the UT in hours (200 = 2h UT). Superimposed on a slow decline, three irregular mini-outbursts of about 0.1 magnitude were recorded. Mrk 421 has been detected as a source of TeV gamma-rays. Miller et al. (1999).

Mark 501

Mark 501

The magnitude variation (unspecified band) for Mrk 501 on 5 June 1998. The x-axis is in days and covers approximately 3 hours. The average level remained constant during this interval, but a 0.1 magnitude mini-outburst was recorded that lasted approximately one hour. A second mini-outburst had apparently begun near the end of the observations. Mrk 501 has been detected as a source of TeV gamma-rays. Miller et al. (1999)

000-017   000-080   000-089   000-104   000-105   000-106   070-461   100-101   100-105  , 100-105  , 101   101-400   102-400   1V0-601   1Y0-201   1Z0-051   1Z0-060   1Z0-061   1Z0-144   1z0-434   1Z0-803   1Z0-804   1z0-808   200-101   200-120   200-125  , 200-125  , 200-310   200-355   210-060   210-065   210-260   220-801   220-802   220-901   220-902   2V0-620   2V0-621   2V0-621D   300-070   300-075   300-101   300-115   300-135   3002   300-206   300-208   300-209   300-320   350-001   350-018   350-029   350-030   350-050   350-060   350-080   352-001   400-051   400-101   400-201   500-260   640-692   640-911   640-916   642-732   642-999   700-501   70-177   70-178   70-243   70-246   70-270   70-346   70-347   70-410   70-411   70-412   70-413   70-417   70-461   70-462   70-463   70-480   70-483   70-486   70-487   70-488   70-532   70-533   70-534   70-980   74-678   810-403   9A0-385   9L0-012   9L0-066   ADM-201   AWS-SYSOPS   C_TFIN52_66   c2010-652   c2010-657   CAP   CAS-002   CCA-500   CISM   CISSP   CRISC   EX200   EX300   HP0-S42   ICBB   ICGB   ITILFND   JK0-022   JN0-102   JN0-360   LX0-103   LX0-104   M70-101   MB2-704   MB2-707   MB5-705   MB6-703   N10-006   NS0-157   NSE4   OG0-091   OG0-093   PEGACPBA71V1   PMP   PR000041   SSCP   SY0-401   VCP550   100-101   70-412   VCP550   LX0-104   000-017   70-461   700-501   70-347   EX200   SSCP   200-120   VCP550   NS0-157   400-201   N10-006   000-080   000-080   70-346   3002   300-101   PMP   640-692   ITILFND   ICBB   70-246   9L0-066