Ehgamberdiev 07082017

High energy astrophysical objects study
at Maidanak observatory in Uzbekistan
Sh. Ehgamberdiev
Ulugh Beg Astronomical Institute of the Uzbekistan Academy of Sciences

At the beginning of 11th century center of Islamic science moved to
Khorezm (Uzbekistan), where such a world known encyclopaedists
as al-Biruni and Ibn Sina (Avicena) worked.

«In 998 AD, two young men living nearly 200 miles apart, in
present-day Uzbekistan, entered into a correspondence. With verbal
jousting that would not sound out of place in a 21st-century
laboratory, they debated 18 questions, several of which resonate
strongly even today».
«Are there other solar systems out among the stars, they asked, or
are we alone in the Universe? In Europe, this question was to
remain open for another 500 years, but to these two men it seemed
clear that we are not alone».
Rediscovering Central Asia, 2009.
S. Frederick Starr. Chairman of the Central Asia-Caucasus Institute at Johns
Hopkins University's School of Advanced International Studies

SN 1006
This is a composite image of the SN 1006 supernova remnant, which is located about 7000 light years from Earth.
Shown here are X-ray data from NASA's Chandra X-ray Observatory (blue), optical data from the University of
Michigan's 0.9 meter Curtis Schmidt telescope at the NSF's Cerro Tololo Inter-American Observatory (CTIO;
yellow) and the Digitized Sky Survey (orange and light blue), plus radio data from the NRAO's Very Large Array
and Green Bank Telescope (VLA/GBT; red).

The Maidanak observatory:
astroclimate and geographic location

Monthly fraction of clear nights
Ehgamberdiev et al, 2000 Astron.Astrophys.Suppl.Ser., v. 145. p.293.

Seeing conditions at Mt. Maidanak
Ehgamberdiev et al, 2000 Astron.Astrophys.Suppl.Ser., v. 145. p.293.

Exploring the Energetic Universe 2017, 7-12 August 2017, Nazarbayev university, Astana, Kazakhstan

The Maidanak observatory: facilities

 6 telescopes: 1.5m, 1m, 4x60cm
 5 CCDs: SI 600 Series 4K,
SITe 2000x800,
2x FLI IMG 1K,
SBIG ST9-XE 0.5K
Direct imaging and photometry (in optic) only, no IR, no Sp.
Maidanak: telescopes and instruments

1.5m instruments
SI600 Series 4Kx4K
Read noise = 4.67 e-
Gain = 1.45 e-/ADU
Dark Curr. = 0.001 e-/pix/sec
Pixel size =15 mkm
Scale = 0.266 (f/7.74)
0.119 (f/17.34)
FOV = 18x18 arcmin
CryoTiger cooled = -108’ C
SITe 2000x800
Read noise = 5.3 e-
Gain = 1.16 e-/ADU
Dark Current = 1 e-/pix/hr
Pixel size = 15 mkm
Scale = 0.266 (f/7.74)
0.119 (f/17.34)
FOV = 8.5x3.5 arcmin
LN2 cooled = -100’ С

Upgrading of the Maidanak’s 1-m telescope

Maidanak: 4 x 0.5-0.6m telescopes

Main fields of scientific research at UBAI
• Gravitationally lensed systems
• AGNs and BL Lac type objects
• Gamma-ray burst afterglows
• Supper Nova
• Open clusters
• Various types of variable stars
• Asteroseismology
• Asteroids: MBA, NEA, young family
• Astroclimate
• Northern Deep Sky Survey
• Astronomical Education
• Relativistic Astrophysics of Gravitational
Compact Objects (BH & NS)

Gravitational Lensing Systems
The GLS project aimed at precise time delay between GLS
components estimation using international collaborative program on
photometry, spectroscopy and astrometry of selected gravitational
lensing systems.
Up to now more or less reasonable Hubble parameter values had been
derived just for 24 GLS (about 10% of all the known perspective
systems). It is important to mention that 7 of them were observed at
Maidanak observatory.

Deconvolution of gravitationaly
lensed quasars
Animation of MCS deconvolution
HE0435-1223 observed at Maidanak
observatory
Results of Maidanak’s images
deconvolution

R-band light curves of the A and B images of UM673 from August 2001 to November
2010. For better representation, the light curve of image B is shifted by -1.87 mag. The
light curves of reference stars 2 and 3 are shown at the bottom. Time delay between
images A and B (image A is leading) and its error appears to be 95 ± 11 days.

GLS H1413+117 (Clover Leaf)
R-band CCD frame of the GLS H1413+117 obtained with the Maidanak
1.5-m telescope, on 2003 February 10. The quasar and the reference stars
R1, R2 and R3 are labelled. The ﬁeld angular size is 2.2’x2.2’.

GLS H1413+117(Clover Leaf)
In case of GLS when components are very close to each other
(dense field) a standard point spread function (PSF) method can
not be applied. For such cases a highly performing photometric
method called the adaptive PSF ﬁtting was developed by Akhunov
et al. (MNRAS 465, 3607–3621, 2017). This method was applied
to GLS H1413+117(Clover Leaf), observed at Maidanak
observatory during observing seasons between 2001 and 2008.

Zoomed R-band images of the central parts of H1413+117. Left: long-focus
mode (pixel size is 0.135”). The seeing is ∼ 0.73” and the image size is
13.5”x13.5”. Right: short-focus mode (pixel size is 0.265”). The seeing is
∼0.66” and the image size is 26.5”x26.5”.

Time delay determinations for GLS H1413+117

Combined light curve of H1413+117. These plots are made from the B, C, D (top) and B,
C (bottom) light curves shifted in time and magnitude with respect to the A component.

Hubble Constant from various lens systems
Oguri M. Gravitational lens time delays: a statistical assessment of lens model
dependences and implications for the global Hubble constant, 2007,ApJ, 660, 1-15
N Lens Name h (1 σ range)
1 B0218+357 0.21 (…)
2 HE 0435-1223 1.02 (0.70–1.39)
3 PXJ 0911+0551 0.96 (0.75–1.21)
4 SBS 0909+532 0.84 (0.47–)
5 FBQ 0951+2635 0.67 (0.56–0.81)
6 Q 0957+561 0.99 (0.82–1.17)
7 HE 1104-1805 1.04 (0.92–1.22)
8 PG 1115+080 0.66 (0.49–0.84)
9 RXJ 1131-1231 0.79 (0.59–1.03)
10 B 1422+231 0.16 (–0.36)
11 SBS 1520+530 0.53 (0.46–0.61)
12 B 1600+434 0.65 (0.54–0.77)
13 B 1608+656 0.89 (0.77–1.20)
14 SDSS J1650+4251 0.53 (0.44–0.63)
15 PKS 1830-211 0.88 (0.58–)
16 HE 2149-2745 0.69 (0.57–0.82)
Average 0.70 (0.68–0.73)

Object (reference for data) Wave
bands
Time delay Reported value
(days)
1 Q0142−100
(Koptelova et al. 2012)
R ∆t AB 89 ± 11
3 HE 0435−1223
(Courbin et al. 2011;
Blackburne et al. 2014)
R ∆t AB
∆t AC
∆t AD
∆t BC
∆t BD
∆t CD
8.4 ± 2.1
0.6 ± 2.3
14.9 ± 2.1
−7.8 ± 0.8
6.5 ± 0.7
14.3 ± 0.8
8 SDSS J1001+5027 (Rathna Kumar et al. 2013) R ∆t AB 119.3 ± 3.3
12 PG 1115+080 (Tsvetkova et al. 2010) R ∆t (A1+A2)B
∆t (A1+A2)C
∆t BC
4.4±3.2
−12±2.5
−16.4±3.5
14 SDSS J1206+4332
(Eulaers et al. 2013)
R ∆t AB 111.3 ± 3
20 SDSS J1650+4251
(Vuissoz et al. 2007)
R ∆t AB 49.5 ± 1.9
24 HS 2209+1914
(Eulaers et al. 2013)
R ∆t AB −20.0 ± 5
S. Rathna Kumar, C. S. Stalin, and T. P. Prabhu
H0 from ten well-measured time delay lenses (A&A 580, A38, 2015)
H0 = 68,1 +-5,9 Km/s Mpc

B L A Z A R S

According to current vision
Blazars are thought to be active
galactic nuclei, with relativistic jets
oriented close to the line of sight
with the Earth. They associated with
a supermassive black hole at the
center of an active, giant elliptical
galaxy.
The special jet orientation explains
the general peculiar characteristics:
high observed luminosity, very
rapid variation, high polarization
(when compared with non-blazar
quasars), and the apparent
supperluminal motions detected
along the first few parsecs of the
jets in most Blazars.
What is Blazar ?

For detailed study of observational properties of
Blazars it is necessary to assemble optical, near-
infrared, millimetre and radio light curves and
investigate their features and correlations. In the optical
band, the spectroscopic and polarimetric observations
can be added. A comparison the low-energy emission
behavior with that at high energies can also provide
very useful information.

Whole Earth Blazar Telescope
The Whole Earth Blazar
Telescope (WEBT) is an
international collaboration of
astronomers organized in
1997 for monitoring blazars
in the optical, near-infrared,
and radio bands.
The WEBT network includes
about 40 optical telescopes,
3 NIR, 8 radio and the Sub-
millimeter Array.

Whole Earth Blazar Telescope
UBAI was involved to WEBT
collaboration in 2000 and since
that they were observed more
than 50 Blazars and identified
the fast optical brightness of 4
Blazars.

List of Blazars observed at Maidanak in 2017
№ Name of
objects
RA DEC Total
observation
nights
Bands
Exposure
(sec)
Total images
1. BL Lac 22:02:43.3 +42:16:40 134 VRI 90+60 1598
2. CTA102 22:32:36.4 11:43:51.3 122 VRI 180 1470
3. 4C38.41 16:35:15.5 +38 08 04 84 VRI 180 1008
4. 3C 371 18:06:50.7 +69 49 28 61 VRI 180 633
5. 3С454.3 22:53:57.7 +16:08:54 101 VRI 180-120 930
6. MRK 501 16:53:52.2 +39:45:37 52 VRI 180 498
7. 3С 66А 02:22:39.6 +43:02:08 85 VRI 120 765
8. 3C 345 16:42:58.8 +39 48 37 45 VRI 180 385
9. 1ES2344 23:47:04.8 +51:42:18 74 VRI 120-180 666
10. PKS1510 15:12:50.5 -09:06:00 35 VRI 180 315
11. PG 026+129 00:29:13.7 +13:16:04 14 VRI 120 140
12. S5 0716 07:21:53.4 +71 20 36 54 VRI 120 486
13. PKS0420 04:23:15.8 −01:20:33 53 VRI 240 477
14. OJ287 08:54:48.9 +20:06:31 15 VRI 180 152

The 4C 38.41 (1633+382) blazar variability study
After years of modest optical activity, the quasar-type blazar 4C 38.41
(1633+382) experienced a big outburst in 2011, which was detected throughout
the entire electromagnetic spectrum, renewing the interest in this source (A&A,
2012, V545, 1).

Optical outburst of CTA 102 Blazar in 2016

The period of relatively low activity has recently been
interrupted by a sudden rise of the source brightness in
late 2016, with a jump of 6–7 magnitudes with respect
to the minima in the optical and near-infrared bands.
The peak of the outburst was observed on December
28, with an R-band magnitude of 10.82 ± 0.04. This
event represents the most luminous optical blazar state
ever detected.
Optical outburst of CTA 102 Blazar in 2016

Conclusion (CTA 102)
The recent unprecedented optical outburst of CTA 102 blazar supports the
picture of an inhomogeneous snaking jet, where photons of different
frequencies come from different regions with different and variable
viewing angles. This is likely caused by MHD instabilities developing
inside the jet, but can also be due to other phenomena, such as jet
precession or orbital motion in a binary black hole system (Nature, 2017,
in press).

Gamma-ray bursts (GRBs) afterglow

Gamma-ray bursts (GRBs) are the
brightest electromagnetic events known to occur in
the Universe. After an initial flash of gamma-rays, a
longer-lived "afterglow" is usually emitted at longer
wavelengths (X-ray, ultraviolet, optical, infrared,
microwave and radio).

GRB follow up collaboration
2001
2003
2005
2006
2005
VT-40/500 (ISON)Shajn, 2.6m
Zeiss-2000
AZT-22, 1.5m
AZT-33IK, 1.6m

Statistics of observations
2003 - 2017
(red – number of bursts; blue – total net exposure; yellow – number of papers)

Statistics of Maidanak GRB observations
2003-2017
GRB/gamma-ray transients observed – 143
Afterglow/host detected – 73
Publications:
In refereed journals – 26
In preparation – 4
Gamma-ray Burst Coordinated Network
circulars (GCN) – 101

Statistics of Maidanak GRB observations
2003-2017
• Net total exposure per year ~ 22 hours
• GRB per year ~ 9
•Mean delay since GRB trigger ~ 6 hours

GRB 130702A afterglow
Monitoring of GRB 130702A afterglow was started
with 1.5-m AZT-22 telescope of the Maidanak
observatory on July 3, 2013, i.e. one and a half days
after the Fermi trigger.

Modelling of the multicolour light curve of
SN 2013dx / GRB 130702A
The light curve of GRB 130702A / SN 2013dx consists of ~320 photometric points, 25 of them are
obtained by AZT-22 telescope of MAO in filters B and R. Our data together with other published
data allowed us to build one of the best-sampled light curves of the SN associated with GRB and to
model it numerically with MHD STELLA code (Volnova et al. MNRAS, 2016)

In our model we obtained the pre-supernova star mass
M = 25 M⊙ and the mass of the resulting compact
remnant MCR = 6 M⊙. Hence, the total mass of the
ejecta was Mej = 19 M⊙. The large ejecta mass and the
possible presence of clumps of matter around the
progenitor (bump in red filters) are consistent with the
explosion of a rather massive star and suggest that the
progenitor of SN 2013dx was a massive Wolf-Rayet
star. The ejecta of a GRB exposes a white dwarf
companion and initiates Type Ia supernova explosion.

Intense Monitoring of Nearby, Bright Galaxies
A primary aim of this project is the study of the early-time
light curve (< 1 day) of supernovae, since such data of SN
can teach us a great deal about the structure of the progenitor
star.

SN 2017ein detected on May 25 in NGC 3938

Ursa Major
It covers 1280 sq. degrees of sky, ranking third in size.

Light curve of SN 2017ein in R-band for period
May 25 till July 24 2017

Preliminary results
NGC 3938 is an unbarred spiral galaxy in the Ursa Major constellation. It was
discovered in 1788 by William Herschel. Four supernova have been identified
within NGC 3938: SN 1961U, SN 1964L, SN 2005ay and SN 2017ein.
SN 2017ein is a type Ic supernova that was discovered on 25 May 2017 and
peaked at magnitude 14.9.
The identification of a progenitor candidate in archival Hubble Space
Telescope (HST) images obtained with the Wide Field Planetary Camera 2
(WFPC2) on 2007 December 11 UT shows that it therefore would be
intrinsically relatively blue and luminous, and could be even bluer and more
luminous with additional reddening internal to the host galaxy (ATel #10485).
Further observations of the SN and analysis of the progenitor candidate are
underway.

Future collaborations
In March 2014 an Agreement between UBAI and National
Astronomical Observatories of the Chinese Academy of Sciences
(NAOC) on upgrading the MAO’s Zeiss-1000 telescope and to
provide during 2017-2022 a large scale sky survey was signed.

The Stellar Abundance and Galaxy Evolution survey
The SAGE survey adopts a new photometric system
(u_s/v_s/g/r/i/ Hαn/Hαw /DDO51 bands), which is extremely
powerful and sensitive to the atmospheric parameters (effective
temperature, gravity and metallicity) of FGK types stars. The
accuracy of the stellar parameters could be higher than that from
the traditional broad-band photometric system or low-resolution
spectra. It is also useful for determination of extinction, stellar
distance, radius, and stellar evolutionary phases.

SAGE Network
Maidanak 1m
Hαn/Hαw/DDO51
Xinjiang 1m griKitt Peak 2.3m u/v

The completeness of SAGE survey
The limiting magnitude could reach 19 mag
in V-band detecting ~0.5 billion stars.

Astronomical Education

Uzbekistan Educational Observatories Layout

GSC 02007-00761 is previously known as a variable star of the
Delta Scuti type. However, the analysis of this light curve
showed that this star is in fact a close binary system.

Andijan University observatory

Thanks for your attention!

Ehgamberdiev 07082017

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