A photometric history of OI 090.4 and OJ-131

Baumert, J. H.

doi:10.1086/130639

Cited by 12 publications

(6 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The polarization is independent of wavelength between the visual and the 2.2µm regions (Craine et al 1978). An optical variation of 2.0 magnitude was found from the examination of the plate archives by Baumert (1980) and a variation of 1 mag in the infrared was reported (CH84). It is the only object in Massaro et al (1995) sample which, despite a recorded variability of about 1 mag, does not show statistically significant changes of the spectral index.…”

Section: Pks 0754+100 Oi 0904mentioning

confidence: 99%

Infrared Variation of Radio‐selected BL Lacertae Objects

Jiang¹,

Lin²

1999

ASTROPHYS J SUPPL S

View full text Add to dashboard Cite

In this paper, the historical infrared (JHK) data compiled from the published literature are presented in electronic form for 40 radio selected BL Lacertae objects (RBLs) for the first time. Largest variations are found and compared with the largest optical variation. Relations between color index and magnitude and between color-color indices are discussed individually. For the color-magnitude relation, some objects ( 0048-097, 0735+178, 0851+202, 1215+303, 1219+285, 1749+096, and perhaps 0219+428, show that color index increases with magnitude indicating that the spectrum flattens when the source brightens while some other objects ( 0754+100, 1147+245, 1418+546, and 1727+502) perhaps show an opposite behaviour, while remaining objects do not show any clear tendency; For color-color relation, it is found common that (J-K) is closely correlated with (J-H) while (J-H) is not correlated with (H-K).Subject headings: Variability-Infrared-BL Lacertae Objects 10, the uncertainty in Col. 9 and 10 is the one sigma deviation. The infrared variations are very large for some objects. The color indices are also variable and associated with the magnitude for some objects, indicating that the spectrum flattens when the source brightens while some objects show different behaviours. For variation, it is reasonable for larger variation to correspond to shorter wavelength, but this paper shows that some objects do show a different behaviour. The objects showing large optical variation also show large infrared variations and high polarizations. Large variation and high polarization are associated. For the color-indices, it is common that there is a correlation for (J-K) and (J-H) while there is almost no correlation for (J-H) and (H-K) although some objects show different properties. But, when the averaged color indices are taken into account, there are mutual correlations between any two color indices of (J-H), (J-K) and (H-K) with the correlation between (J-H) and (H-K) being not so close as compared with other two correlations. (J-K) = 2.26(J-H) -0.28 with correlation coefficient r = 0.90 and the probability of chance correlation p = 6.3 × 10 −11 , (H-K) = 1.44(J-H) -0.41 with r = 0.80and p = 4.4 × 10 −7 , and (J-K) = 1.62(H-K) + 0.33 with r = 0.93 and p = 6.1 × 10 −13 . The (J-H) and (H-K) relation is shown in Fig. 1. In the next section, individual objects are discussed. Remarks PKS 0048-097, OB − 081, MC3, P HL856There is no redshift available for this polarized ( P 3.7cm = 9.3%, Wardle 1978;P opt =1%-27 %, CH(84); Brindle et al. 1986 ) object. Very faint infrared fluxes have been observed by Gear (1993), which leads the object to have the largest infrared variation among the objects discussed in the present paper. The infrared variations are ∆J = 6.55, ∆H = 6.23, and ∆K = 6.07 while that in the optical band is 2.7 mag (Angel & Stockman 1980). We can expect that the optical monitoring should get a similar amplitude. For color-color indices, there are correlations for (J-K) and (J-H) and for (J-K) and (H-K):(J-K) = 1.20(J-H) +...

show abstract

Section: Pks 0754+100 Oi 0904mentioning

confidence: 99%

Infrared Variation of Radio‐selected BL Lacertae Objects

Jiang¹,

Lin²

1999

ASTROPHYS J SUPPL S

View full text Add to dashboard Cite

show abstract

“…OI 090.4 (PKS 0754+110) was identified as a BL Lacobject by Tapia et al (1977). Its historical light curve has been studied by Baumert (1980), who found 0.8 mag variations on timescales of a few days and a variability of 2 mag in a few years. Pica et al (1988) observed 0.8 magnitude (B-band) changes on a 2 year timescale.…”

Section: Pks 0736+107mentioning

confidence: 99%

Tuorla quasar monitoring

Katajainen

Takalo

Sillanpää

et al. 2000

Astron. Astrophys. Suppl. Ser.

View full text Add to dashboard Cite

Abstract. We present results of optical monitoring of quasars and blazars obtained at Tuorla Observatory between September 1995 and May 1997. The aim of our monitoring is to provide well sampled optical light curves for quasar and blazar studies. During the observing period the V -band brightness of S2 0109+224, 3C 66A, and ON 231 (W Comae) reached some of the brightest values ever measured for these objects. A strong outburst was observed in Mrk 421 and the large outburst, which was predicted earlier, in OJ 287 was confirmed. CTA 102 had over one magnitude outburst which happened in a timescale of a few days. For OI 090.4 we measured one of the faintest V -band brightness values ever.

show abstract

“…Falomo et al (1993a) observed this blazar in the optical-near IR and did not detect a significant contribution of the host galaxy. An archival research using the Harvard plate collection (Baumert 1980) showed significant rapid optical flares of ∼ 0.8 mag with time scales ranging from a few days to one month. Flickering of about 0.8 mag superimposed on long term trends spanning 1-2 years was also observed by Pica et al (1988).…”

Section: Notes On Individual Objectsmentioning

confidence: 99%

Automatic optical monitoring of 10 blazars

Fiorucci

Tosti

1996

Astron. Astrophys. Suppl. Ser.

View full text Add to dashboard Cite

Abstract. -We report the BV RcIc data for 10 blazars observed in the first phase of a long-term photometric monitoring program of about 30 objects. The observations were carried out with a 0.40-m automatic imaging telescope, recently developed by our group at the Perugia University Observatory. During our period of observation 1215+303 and 1424+240 were at their highest values of magnitude, while 0754+100 and 0829+043 displayed large amplitude flares. We further report optical data of Mrk 501 during the same period in which TeV γ-rays were detected by the Whipple Observatory.

show abstract

A photometric history of OI 090.4 and OJ-131

Cited by 12 publications

References 0 publications

Infrared Variation of Radio‐selected BL Lacertae Objects

Infrared Variation of Radio‐selected BL Lacertae Objects

Tuorla quasar monitoring

Automatic optical monitoring of 10 blazars

Contact Info

Product

Resources

About