V. Lipunov

V. Kornilov

E. Gorbovskoy

K. Zhirkov

N. Tyurina

P. Balanutsa

A. Kuznetsov

V. Senik

D. Vlasenko

G. Antipov

D. Zimnukhov

E. Minkina

A. Chasovnikov

V. Topolev

D. Kuvshinov

D. Cheryasov

Ya. Kechin

Yu. Tselik

A. Sosnovskij

R. Podesta

C. Lopez

F. Podesta

C. Francile

R. Rebolo

M. Serra

D. Buckley

O. A. Gress

N. M. Budnev

O. Ershova

L. Carrasco

J. R. Valdes

V. Chavushyan

V. M. Patino Alvarez

J. Martinez

A. R. Corella

L. H. Rodriguez

A. Tlatov

D. Dormidontov

V. Yurkov

A. Gabovich

MASTER-Tavrida robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the Swift GRB230913.70 (trigger No 1191903, 19h 58m 46.70s, +35d 26m 01.0s, R=0.05) error box 19 sec after notice time and 102 sec after trigger time at 2023-09-13 16:45:58 UTC, with upper limit up to 15.6 mag. Observations started at twilight. The observations began at zenith distance = 18 deg. The sun altitude is -9.3 deg. 

The galactic latitude b = 3 deg., longitude l = 72 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2269973

We obtain a following upper limits.

```
Tmid-T0  |          Site       |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________

     113 |      MASTER-Tavrida |   C |    20 | 15.2 |        
     146 |      MASTER-Tavrida |   C |    30 | 15.5 |        
     190 |      MASTER-Tavrida |   C |    10 | 15.1 |        
     201 |      MASTER-Tavrida |   C |    10 | 15.1 |        
     222 |      MASTER-Tavrida |   C |    20 | 15.5 |        
     243 |      MASTER-Tavrida |   C |    20 | 15.5 |        
     265 |      MASTER-Tavrida |   C |    20 | 15.5 |        
     291 |      MASTER-Tavrida |   C |    30 | 15.6 |     
   
     Filter C is a clear (unfiltred) band. 
```

The observation and reduction will continue. The message may be cited.

MASTER

Fermi-LAT gamma-ray observations of IceCube-220822A and detection of a new gamma-ray source, Fermi J1810.1+2154

O.A. Gress

The high redshift (z~2.1) flat spectrum radio quasar (FSRQ) 4C+01.02 **(ICRS coordinate. (ep=J2000): RA 01 08 38.77, Dec +01 35 00.3)** was observed by Fermi-LAT in gamma-ray (>100 MeV) in high activity state (https://fermi.gsfc.nasa.gov/FTP/glast/data/lat/catalogs/asp/current/lightcurves/4C+01.02 86400 1yr.png). Following the gamma-ray bright state, X-ray observations of the source were triggered with Swift-XRT. The proposed observation was conducted from September 1, 2022 (11:52:00 UTC), to September 2, 2022 (08:34:00 UTC), in the photon counting (PC) mode for a net exposure of 1.1 Ks. The ToO observation suggests that the source is in the bright state in the X-ray band. The preliminary analysis has been performed fitting the X-ray spectrum with an absorbed power-law considering the galactic absorption corresponding to hydrogen column density of N_H=2.42 x 10^20 cm^-2 (Kalberla et al. 2005, A&A, 440, 775). The observed X-ray (0.3-10 keV) flux on September 1, 2022, is found to be 4.21(+0.80,-0.80) x 10^-12 erg cm^-2 s^-1 is one of the highest flux states of the source. The power law spectral index during this observation is 1.43 (+0.41, -0.41). In light of ongoing activity in Swift-XRT, we encourage further multiwavelength observation of 4C+01.02 (PKS 0106+01, OC 12). We thank the Swift Team and Observatory Duty Scientists who made these observations possible.

MASTER-Amur Robotic Telescope

Swift XRT observations of the high redshift (z=2.1) flat spectrum radio quasar 4C+01.02

Anton

Lorem ipsum dolor sit amet, consectetur adipiscing elit. Quisque sollicitudin rutrum interdum. Nullam sollicitudin eros et risus porttitor, vel viverra eros tempus. In ac sem venenatis, pellentesque massa eget, pellentesque neque. Fusce et ligula quis turpis facilisis dapibus fringilla luctus ante. Curabitur scelerisque ipsum non faucibus consequat. Donec fringilla ex fringilla felis rhoncus eleifend.

This is supertest

### Mathematics -->

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Goophy

MASTER OT J172704.87-163544.4 discovery

V.Lipunov (Lomonosov MSU), E.Gorbovskoy, N.Tiurina, P.Balanutsa, A.Kuznetsov,
V.Kornilov, O.Gress, K.Ivanov, V.Vladimirov, D.Kuvshinov (Lomonosov Moscow
State University, SAI)

MASTER-OAFA auto-detection system ( Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 30L )
 discovered OT source at (RA, Dec) = 17h 27m 04.87s -16d 35m 44.4s on 2023-09-16.11803 UT.

The OT magnitude in 'BLANK' filter is 16.6m
(mlim16.4=).

The OT is seen in 38 images. There is no minor planet at this place.

We have reference image on 2018-04-16.25163 UT with 'BLANK' filter 18.1m.

Spectral observations are required.


NASA

Привет!

The high redshift (z~2.1) flat spectrum radio quasar (FSRQ) 4C+01.02 (ICRS coordinate. (ep=J2000): RA 01 08 38.77, Dec +01 35 00.3) was observed by Fermi-LAT in gamma-ray (>100 MeV) in high activity state (https://fermi.gsfc.nasa.gov/FTP/glast/data/lat/catalogs/asp/current/lightcurves/4C+01.02 86400 1yr.png). Following the gamma-ray bright state, X-ray observations of the source were triggered with Swift-XRT. The proposed observation was conducted from September 1, 2022 (11:52:00 UTC), to September 2, 2022 (08:34:00 UTC), in the photon counting (PC) mode for a net exposure of 1.1 Ks. The ToO observation suggests that the source is in the bright state in the X-ray band. The preliminary analysis has been performed fitting the X-ray spectrum with an absorbed power-law considering the galactic absorption corresponding to hydrogen column density of N_H=2.42 x 10^20 cm^-2 (Kalberla et al. 2005, A&A, 440, 775). The observed X-ray (0.3-10 keV) flux on September 1, 2022, is found to be 4.21(+0.80,-0.80) x 10^-12 erg cm^-2 s^-1 is one of the highest flux states of the source. The power law spectral index during this observation is 1.43 (+0.41, -0.41). In light of ongoing activity in Swift-XRT, we encourage further multiwavelength observation of 4C+01.02 (PKS 0106+01, OC 12). We thank the Swift Team and Observatory Duty Scientists who made these observations possible.

O.Ershova

MASTER-Tavrida auto-detection system ( Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 30L )
 discovered OT source at (RA, Dec) = 00h 41m 22.44s +40d 56m 37.9s on 2023-09-13.94319 UT.

The OT magnitude in 'FAULT' filter is 18.4m
(mlim19.6=).

The OT is seen in 12 images. There is no minor planet at this place.

We have reference image on 2023-08-27.99131 UT with 'FAULT' filter 19.8m.

Spectral observations are required.


MASTER OT J004122.44+405637.9 discovery

Following the announcement of a new outburst of the symbiotic star V919 Sgr (Munari et al., ATel #15528), on 2022 July 31 we observed V919 Sgr with the Swift satellite. The pointing started at 13:57 UT. The source was well detected in all UVOT filters, yielding the Vega-system magnitudes reported in the Table below (errors +/-0.07 mag). It was instead not detected in X-rays: a simultaneous XRT observation lasting about 1700 s did not reveal any emission in the 0.3-10 keV band down to a 3-sigma limit of 3.3x10-3 counts s-1. For the distance and reddening listed below, and assuming a kT=0.1 keV bremsstrahlung, this corresponds to <4x10-13 erg/cm2/s in flux and <1x1033 erg/s in LX luminosity.




    To extend the photometric coverage to the optical range, we also observed V919 Sgr with the Asiago 67/92cm Schmidt telescope. The resulting UBVRI magnitudes are listed in the table below (errors <0.005 mag). We have also obtained on Aug 5.959 UT a near-UV, medium-resolution, high S/N spectrum of V919 Sgr with the Asiago 1.22m+B&C telescope, covering the 3190-4400 Ang at 0.58 Ang/pix. The only feature visible in emission is a feeble Hgamma, with Hdelta exactly filling the absorption from the underlying continuum spectrum which is best described as a forest of very sharp absorption atomic lines, so tightly packed that the "true" continuum emerges only at a few pixels sparsely distributed over the recorded spectral interval.




    2022 UT UVW2  UVM2  UVW1  U B V R I
    Jul 31.581        12.63   12.78   11.89         
    Aug 02.904        11.004  11.127  10.573  10.056  9.313
    Aug 03.905        10.988  11.125  10.563  10.051  9.311
    The distance to V919 Sgr is determined by Gaia DR3 in 4.6 kpc (4.0-5.5 kpc limits). The high Galactic latitude (-10deg) favors a low reddening, determined in E(B-V)=0.19 by averaging the results of Marshall et al. (2006, A&A 453, 635) and Green et al. (2019, ApJ 887, 93). After subtracting the contribution of the non-variable M3III giant and dereddening by E(B-V)=0.19, the luminosity radiated by the hot component in the UVOT-UBVRI range is 4.27 x 1036 erg/s (3.20 x 1036 and 5.96 x 1036 at lower and upper limits to Gaia distance). V919 Sgr belongs to the group of symbiotic stars characterized by stable nuclear burning on the surface of the WD. The large luminosity radiated at optical and near-UV wavelengths during the present outburst (1100 Lsun) and the drastic drop in the ionization conditions described by Munari et al. (ATel #15528), support the idea that the outburst was caused by a shift toward optical wavelengths of the emission from the WD, driven by an expansion in radius of its burning shell and fueled by a possible surge in mass-transfer from the M3III companion or the accretion disk.




    Flickering is ubiquitous in accreting-only symbiotic stars (Luna et al. 2013, A&A 559, A6) and absent for the burning variety (Sokoloski 2003, ASPC 303, 202). During the UBVRI observations of V919 Sgr on Aug 2 and 3, we have collected sparse U-band data distributed over 1.5 hours intervals on both nights, and found the U-band brightness stable to better than 0.01 mag. The absence of flickering agrees with the inferred nuclear burning on the WD.




    We thank the Swift Team for the quick approval, scheduling and acquisition of the observation presented in this communication.

Luminosity radiated by the symbiotic star V919 Sgr in outburst, as derived from ground-based and Swift observations

Negoro et al (ATel #15586) report the MAXI detection of an outbursting source in M15. On September 3rd, 2022 at 13:09UT, Swift performed a target-of-opportunity observation of the source, with a 1ks observation taken with XRT in Photon Counting (PC) mode. We find a bright source at the following location: RA/Dec(J2000) = 322.49242, 12.16698 which is equivalent to: 




    RA(J2000) = 21h 29m 58.18s, 
    Dec(J2000) = +12d 10m 01.1s, 




    with an error radius of 2.4 arc-seconds (90% confidence). We note that this position lies 2.3 arc-seconds from M15 X-2, consistent with its location, AC211 lies 2.6 arc-seconds from this position just outside of the error circle (positions from White and Angelini, 2001). Therefore, we cannot from these data alone identify which of these sources are in outburst.




    The spectrum of is well fit by an absorbed power-law model with absorption N_H = 2.0 +/- 0.3 x 10^21 cm^-2 and photon index 1.89 +/- 0.1. The flux, corrected for pile-up and absorption is 1.54 +/- 0.08 x 10^-9 erg/s/cm^2 (0.3 - 10 keV , which is equivalent to a luminosity of ~2 x 10^37 erg/s (0.3 - 10 keV) assuming an 10.9 kpc distance to M15.

Swift confirms outburst of transient in M15

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