Insights into the broadband emission of the TeV blazar Mrk 501 during the first X-ray polarization measurements

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Volume 685 (May 2024)

A&A, 685 (2024) A117

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Table 1.

Parameters for the VHE and X-ray observations around the three IXPE pointings.

	Observations	IXPE-1			IXPE-2			IXPE-3
	MJD	59 646.11 to 59 648.35			59 665.24 to 59 667.30			59 769.97 to 59 772.04

MAGIC	MJD	59 645.24 to 59 649.25			59 664.19 to 59 669.19			59 769.10 to 59 769.11
	Flux	0.45 ± 0.03			0.73 ± 0.04			0.32 ± 0.01
	α	2.47 ± 0.04			2.44 ± 0.04			2.50 ± 0.24
	χ²/d.o.f.	22.15/14			22.15/14			5.10/4

LAT	MJD	59 640.23 to 59 654.23			59 659.27 to 59 673.27			59 764.01 to 59 778.01
	Flux	2.55 ± 1.24			1.74 ± 0.74			1.00 ± 0.31
	α	1.60 ± 0.13			1.80 ± 0.14			2.10 ± 0.17

NuSTAR	MJD	59 647.42 to 59 647.88			59 665.06 to 59 665.55			(...)
	Flux	0.784 ± 0.003			1.135 ± 0.004			(...)
	α	1.851 ± 0.007			1.684 ± 0.005			(...)
	χ²/d.o.f.	951.6/925			1150.2/1123			(...)

Swift-XRT	MJD	59 646.13	59 646.21	59 647.13	59 664.18	59 665.16	59 666.16	59 770.16	59 771.15
	Flux	$1 . 51_{- 0.05}^{+ 0.06}$ $1.51^{+0.06}_{-0.05}$	$1 . 51_{- 0.05}^{+ 0.06}$ $1.51^{+0.06}_{-0.05}$	$1 . 37_{- 0.05}^{+ 0.05}$ $1.37^{+0.05}_{-0.05}$	$1 . 98_{- 0.06}^{+ 0.06}$ $1.98^{+0.06}_{-0.06}$	$2 . 00_{- 0.06}^{+ 0.06}$ $2.00^{+0.06}_{-0.06}$	$2 . 53_{- 0.07}^{+ 0.07}$ $2.53^{+0.07}_{-0.07}$	$1 . 05_{- 0.04}^{+ 0.04}$ $1.05^{+0.04}_{-0.04}$	$1 . 06_{- 0.04}^{+ 0.05}$ $1.06^{+0.05}_{-0.04}$
	α	$1 . 95_{- 0.02}^{+ 0.02}$ $1.95^{+0.02}_{-0.02}$	$1 . 95_{- 0.02}^{+ 0.02}$ $1.95^{+0.02}_{-0.02}$	$2 . 01_{- 0.02}^{+ 0.02}$ $2.01^{+0.02}_{-0.02}$	$1 . 90_{- 0.02}^{+ 0.02}$ $1.90^{+0.02}_{-0.02}$	$1 . 90_{- 0.02}^{+ 0.02}$ $1.90^{+0.02}_{-0.02}$	$1 . 84_{- 0.02}^{+ 0.02}$ $1.84^{+0.02}_{-0.02}$	$2 . 16_{- 0.02}^{+ 0.02}$ $2.16^{+0.02}_{-0.02}$	$2 . 12_{- 0.02}^{+ 0.02}$ $2.12^{+0.02}_{-0.02}$
	χ²/d.o.f.	258.5/212	268.28/219	221.22/217	331.22/253	271.97/241	266.25/274	190.39/195	192.28/181
	MJD	59 647.20		59 648.12	59 667.23		59 669.14	(...)
	Flux	$1 . 45_{- 0.04}^{+ 0.05}$ $1.45^{+0.05}_{-0.04}$		$1 . 09_{- 0.04}^{+ 0.05}$ $1.09^{+0.05}_{-0.04}$	$2 . 70_{- 0.07}^{+ 0.07}$ $2.70^{+0.07}_{-0.07}$		$2 . 17_{- 0.06}^{+ 0.05}$ $2.17^{+0.05}_{-0.06}$	(...)
	α	$1 . 98_{- 0.02}^{+ 0.02}$ $1.98^{+0.02}_{-0.02}$		$2 . 02_{- 0.02}^{+ 0.02}$ $2.02^{+0.02}_{-0.02}$	$1 . 82_{- 0.01}^{+ 0.01}$ $1.82^{+0.01}_{-0.01}$		$1 . 88_{- 0.01}^{+ 0.01}$ $1.88^{+0.01}_{-0.01}$	(...)
	χ²/d.o.f.	232.89/220		216.78/197	292.01/289		307.98/278	(...)

Notes. Stated are the MJD of the observations, the flux values in 10⁻¹⁰ erg cm⁻² s⁻¹ (for MAGIC with E > 200 GeV; for Fermi-LAT from 0.3 − 300 GeV; for XRT from 2 − 10 keV; from 3 − 7 keV for NuSTAR), the spectral index α and the χ²/d.o.f. for the spectral fits. For all wavebands, a simple power law was used as a spectral model (with a normalization energy of 300 GeV for MAGIC, 1 GeV for Fermi-LAT and 1 keV for Swift-XRT) because there is no significant preference for a log-parabola function, except for the NuSTAR data. The NuSTAR fits are performed using a log-parabola model with a curvature parameter fixed to 0.3 (and normalization energy at 1 keV).

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