P. Magdziarz's research while affiliated with Jagiellonian University and other places

... At a distance of ∼15.8 Mpc (e.g., Yuan et al. 2020), NGC 4151 is also one of the most intensively studied nearby AGNs across the electromagnetic spectrum (e.g., Crenshaw et al. 1996;Edelson et al. 1996;Kaspi et al. 1996;Warwick et al. 1996;Kraemer et al. 2005;Wang et al. 2011;Bon et al. 2012;Williams et al. 2017;Lyu & Rieke 2021). NGC 4151 is bright, highly variable and has been previously monitored by a number of RM campaigns (Clavel et al. 1990;Ulrich & Horne 1996;Maoz et al. 1991;Kaspi et al. 1996;Bentz et al. 2006;De Rosa et al. 2018). ...

... Austin, these values are re-evaluations of the ones of Crovisier et al. (1993). For the preperihelion phase, we found 48 values of CN production rates (Schleicher et al., 1991 andMagdziarz et al., 1995). Like comet Austin, comet Levy appeared during the maximum of the solar activity, thus, for the re-evaluation of CN production rates, we have used exactly the same parameters than for comet Austin. ...

... Our results are in agreement with those of Waniak et al. (1994). These authors also found that C2 production rate decreases with the increasing heliocentric distance not so rapidly as the CN production rate. ...

... The By combining observations in different energy bands, a picture has emerged where the overall shapes of the X-ray and γ-ray spectra of different Seyfert 1 galaxies are similar. The only Seyfert 1 galaxy for which the broad band X-and γ-ray spectrum is well determined is IC 4329A (Madejski et al. 1995) being the second brightest Seyfert galaxy in the 2-10 keV range. Simultaneous ROSAT and CGRO OSSE, as well as nonsimultaneous Ginga data are shown inFigure 1 (left panel). ...

... Equally important in deriving the physical properties of the disk and corona is the selection of a representative, bright target. One good candidate is the southern Seyfert 1.2 galaxy IC 4329A (z = 0.0161, Willmer et al. 1991; N H [gal] = 4.61 × 10 20 cm −2 , Kalberla et al. 2005; M BH = 1.20 × 10 8 M ⊙ , de La Calle Pérez et al. 2010), which in the hard Xray/soft γ-ray band appears similar to an average radio-quiet Seyfert (e.g., Zdziarski et al. 1996). The host galaxy is an edge-on spiral in a pair with IC 4329, separated by ∼ 3 arcmin. ...

... However, we know that the reflection spectrum is a modified continuum with multiple atomic emission lines hence a full reflection model framework should be used to properly describe all the reprocessed emission. Eventually more sophisticated model grids were developed that encompassed the reprocessed continuum from irradiation of a constant density medium with varying illumination continua (Magdziarz and Zdziarski 1995;Ross et al. 1999;García and Kallman 2010;García et al. 2011García et al. , 2013García et al. , 2022. Additionally, ad-hoc convolution reflection models were created that piece together expected shapes in different energy bands, such as RFXCONV (Done and Gierliński 2006;Kolehmainen et al. 2011), which generates an angle-dependent reflection spectrum from a Comptonized input spectrum by combining the reflection emission from an ionized disk interpolated from REFLIONX (Ross and Fabian 2005) below 14 keV (using the average 2-10 keV power-law index) with Compton reflected emission from PEXRIV (Magdziarz and Zdziarski 1995) above 14 keV (using the average 12-14 keV power-law index). ...

... However, Ecut measurements are difficult to obtain due to the requirement of X-ray data with high S/N beyond 10 keV. In spite of that, Ecut measurements for few nearby AGN are available via analysis of data from the Compton Gamma Ray Observatory (CGRO; Zdziarski et al. 2000Zdziarski et al. , 1996Johnson et al. 1997), BeppoSAX (Nicastro et al. 2000;Dadina 2007), INTEGRAL (Malizia et al. 2014;Lubiński et al. 2010Lubiński et al. , 2016Ricci et al. 2011), Swift/BAT (Vasudevan et al. 2013a;Ricci et al. 2017) and Suzaku (Tazaki et al. 2011). The launch of the Nuclear Spectroscopic Telescope Array (NuSTAR; Harrison et al. 2013) with its unique capability to focus hard X-rays and thereby providing good signal to noise ratio data in the 3−79 keV band has allowed us to get improved values of Ecut measurements for a growing number of AGN. ...

... To check the temporal variability of Mrk 6 across different energy bands, we calculate the fractional variability F var (Edelson et al. 1996 ;Nandra et al. 1997 ;Rodr íguez-Pascual et al. 1997 ;Vaughan et al. 2003 ;Edelson & Malkan 2012 ). The fractional variability for a light curve of x i counts/s with the measurement error σ i for N number of data points, mean count rate μ and standard deviation σ , is given by the relation, ...

... Furthermore, warm coronae (kT e ∼ 1 keV, τ T ? 1) on top of optically thick accretion disks have been invoked to explain soft X-ray excesses found in many AGNs (e.g., Magdziarz et al. 1998;Petrucci et al. 2020;Ursini et al. 2020;Xiang et al. 2022). Analogous soft X-ray excesses were also found in some BH XRBs, in particular in the soft state of GRS 1915 + 105 (a low-mass BH XRB), which was fitted by hybrid Comptonization including a low-temperature, high optical depth, thermal component (Zdziarski et al. 2001). ...

... X-rays emitted on the far side of the stream (with respect to the observer) encounter a larger effective column-density to the observer compared to those emitted on the side facing the observer. To account for this we convolve cemekl with the absorption model pwab (Done & Magdziarz 1998), which calculates the emission assuming the non-uniform absorption profile arising from a cylindrical emitter. We further convolve the model with relfect (Magdziarz & Zdziarski 1995), which calculates the reflected emission from neutral material. ...