Determining the Microlens Mass Function from Quasar Microlensing Statistics
نویسندگان
چکیده
The first investigations of the response of the microlensing magnification pattern (at an optical depth of order unity) to the mass function of the microlenses found that the resulting statistics depend only on the mean microlens mass 〈m〉. In particular the mean microlensing caustic crossing rate was found to be proportional to
منابع مشابه
Unambiguous quasar microlensing
Microlensing studies of quasars can reveal dark matter lumps over a broad mass spectrum; we highlight the importance of monitoring quasars which are seen through the halos of low-redshift galaxies. For these configurations microlensing by planetary-mass objects will manifest itself as isolated events which are only weakly chromatic. Statistical comparison of the observed optical depths with the...
متن کاملOn the contribution of microlensing to X-ray variability of high-redshifted QSOs
We consider a contribution of microlensing in X-ray variability of high-redshifted QSOs. Such an effect could be caused by stellar mass objects (SMO) located in a bulge or/and in a halo of this quasar as well as at cosmological distances between an observer and a quasar. Here, we not consider microlensing caused by deflectors in our Galaxy since it is well-known from recent MACHO, EROS and OGLE...
متن کاملMicrolensing of Quasars
There are two possible causes of variability in gravitationally lensed quasars: intrinsic fluctuations of the quasar and “microlensing” by compact objects along the line of sight. If disentangled from each other, microlens-induced variability can be used to study two cosmological issues of great interest, the size and brightness profile of quasars on one hand, and the distribution of compact (d...
متن کاملEvidence for a source size of less than 2000 AU in Quasar 2237+0305
Recently, OGLE team have reported clear quasar microlensing signal in Q2237+0305. We have analyzed the microlens event of “image C” by using their finely and densely sampled lightcurves. From lightcurve fitting, we can unambiguously set the source size of < ∼ 0.98 Einstein Ring radius as a conservative limit. This limit corresponds to 2000(AU), if we adopt Mlens ∼ 0.1M obtained by a recent stat...
متن کامل35 8 v 1 2 1 Se p 19 99 Determination of the transverse velocity of Q 2237 + 0305
The largest systematic uncertainty present in the analysis of gravitationally microlensed quasar light curves is that of the galactic transverse velocity. We describe a method for determining the transverse velocity as well as its application to published monitoring data of Q2237+0305 (Irwin et al. 1989; Corrigan et al. 1991; Østensen et al 1995). We find that while this data displays strong ev...
متن کامل