The HE/UHE astrophysical sources The HE/UHE astrophysical sources - - PowerPoint PPT Presentation

Ren René é Hudec and collaborators Hudec and collaborators

Astronomical Institute, Academy of Astronomical Institute, Academy of Sciences Sciences 251 65 Ondrejov, Czech Republic 251 65 Ondrejov, Czech Republic

1 Vulcano Workshop 2010

The HE/UHE astrophysical sources The HE/UHE astrophysical sources as optical emitters: monitoring as optical emitters: monitoring efforts and spectral analyses efforts and spectral analyses

Why optical monitoring of Why optical monitoring of HE/UVE sources HE/UVE sources

 Multispectral analyses for good science. Very common is the

situation when we have satellite/HE monitoring data covering up to ~ years, but we do not have simultaneous optical data

 Important goal is to recognize active states of the sources (flares,

high states, etc) either to trigger the satellite or TeV

• bservations, or, alternatively, to be able to concentrate of

archival satellite data for that’s periods

2 Vulcano Workshop 2010

• I. Dedicated Monitoring
• I. Dedicated Monitoring

 In this regime, the narrow field telescopes

• bserve the target frequently

 Important goal for robotic telescopes

3 Vulcano Workshop 2010

• II. The Non-Dedicated Optical
• II. The Non-Dedicated Optical

Monitoring Monitoring

 In this regime, wide-field or all-sky optical images are

stored covering large numbers of objects

 The monitors can deliver optical photometric data for

• bjects prior and during the active/flaring states – WF

coverage is important to cover as much sources as possible

 Photographic Sky Patrols (2 still in operation)  All-Sky and Wide-Field CCD cameras  Various survey projects

4 Vulcano Workshop 2010

The importance of optical The importance of optical monitoring for ESA monitoring for ESA INTEGRAL INTEGRAL

 Hard X-ray and gamma-ray sources

typically 10-80 keV

 Examples: Cataclysmic Variables, Blazars

Vulcano Workshop 2010 5

B B magnitud

V V magnitud

Legend - B 1 = 2,29 - 5 2 = 5 -10 3 = 10 - 15 4 = 15 - 20 5 = 20 - 23 Legend - V 1 = 2,39 - 5 2 = 5 -10 3 = 10 - 15 4 = 15 - 20 5 = 20 - 21

Optical B and V magnitudes of optically identified INTEGRAL Optical B and V magnitudes of optically identified INTEGRAL gamma-ray sources gamma-ray sources … … most are brighter than mag 20, and most are brighter than mag 20, and more than half more than half are brighter are brighter than mag 15 than mag 15

>90% brighter than mag 20

Even gamma-ray sources do have optical counterparts accessible by optical telescopes

6 Vulcano Workshop 2010

V834 Cen in optical high and low state V834 Cen in optical high and low state

IBIS image at optical active IBIS image at optical active state state 14 mag 14 mag Object detected Object detected IBIS image at optical low state IBIS image at optical low state 17 mag 17 mag Object not detected Object not detected It can be an explanation why some CV are visible and some not It can be an explanation why some CV are visible and some not

7 Vulcano Workshop 2010

It s It shows hows active active and and in ina active ctive states

• states. Optical monitoring

. Optical monitoring

• f sources is important as it can indicate active
• f sources is important as it can indicate active

intervals when the object is expected to be active also intervals when the object is expected to be active also in gamma-rays in gamma-rays

This polar was probably detected by This polar was probably detected by IBIS since it was in high (active) state IBIS since it was in high (active) state. .

Comparing optical and gamma-ray activity is difficult Comparing optical and gamma-ray activity is difficult in most ca in most cas ses due to lack of optical ( es due to lack of optical (!) data. !) data. Goal for Goal for robotic telescopes. robotic telescopes.

INTEGRAL IBIS gamma-ray images

1ES 1959+650 1ES 1959+650 variable blazar visible in gamma-

variable blazar visible in gamma- rays by INTEGRAL IBIS only during rays by INTEGRAL IBIS only during

• ptical flare
• ptical flare

MJD interval 53416.96-53792.96 i.e. 376.00 days [Feb 2006 - Feb 2007]

Optical LC IBIS LC

8 Vulcano Workshop 2010 MJD interval 52985.52-53203.34 i.e. 217.82 days [Dec 2004 - Jul 2005]

INTEGRAL IBIS gamma-ray images

Vulcano Workshop 2010 9

The VHE Sky The VHE Sky

The VHE sky is dominated by objects which are (in many cases) also The VHE sky is dominated by objects which are (in many cases) also sources of optical emission sources of optical emission

Vulcano Workshop 2010 10

Multispectral Multispectral Approach Approach Typical SEDs Typical SEDs

• f some of the
• f some of the

TeV sources TeV sources TeV sources TeV sources expected to be expected to be bright optical bright optical sources sources

Energy range Energy range covered by optical covered by optical data data

Vulcano Workshop 2010 11

….. and some optical magnitudes of TeV sources … many do have bright optical emission

LSI +61 303 mag_v 10.8 HESS J0632+058 mag_v 9.08 Centaurus X3 mag_v 13.25 PSR B1259-63 mag_v 10.68 HESS J1747-281 mag_v 9.25 HESS J1825-137 mag_v 11.4 LS 5039 mag_v 11.23 These sources can be in optical light accessed by small telescopes and cameras

Gamma-Ray Binaries Gamma-Ray Binaries

 γ-ray binaries: new class of objects with emission

extending from radio to TeV

 LS I +61 303 has been detected at TeV energies by

MAGIC:

– The emission is variable – Possible hint of periodicity – The maximum of the emission happens 1/3 of the orbit away

from periastron

 The emission produced by electrons accelerated in the

interaction of the stellar and the pulsar winds.

 New MAGIC+multi-wavelength observations will study

deeper the TeV emission (periodicity? Intra-night variability?) and correlations with radio and x-ray emissions.

Vulcano Workshop 2010 12

Examples of TeV Blazars Examples of TeV Blazars in Multispectral Approach in Multispectral Approach

 Need to improve optical monitoring to be able to

provide high-quality LCs for multi-spectral analyses

 Goal for robotic telescopes  We also need an alert system analogous to these

used in GRB satellites to provide fast response to TeV flares

Vulcano Workshop 2010 13

Vulcano Workshop 2010 Ciro Bigongiari 14/23

1ES1959+650(z=0.047) 1ES1959+650(z=0.047)

• Blazar famous for the orphan flare in 2002

Blazar famous for the orphan flare in 2002

• MAGIC: Significant signal

MAGIC: Significant signal in only 6h of effective obs. in only 6h of effective obs. time ApJ, 639 (2006), 761. Lack of optical data! time ApJ, 639 (2006), 761. Lack of optical data! TeV TeV X-ray X-ray Opt. Opt.

Mkn 421 2008 flare Mkn 421 2008 flare

Vulcano Workshop 2010 15

a) R-band optical light curve from GASP-WEBT (May 24–June 23); b) ASM (2-12 keV) light curve (bin size is 1 day) and XRT (2-10 keV) flux (blue triangle); c) SuperAGILE (20-60 keV, blue triangles; 1 Crab = 0.2 ph cm−2 s−1) and BAT (15-50 keV, empty black squares; 1 Crab = 0.29 ph cm−2 s−1); d) MAGIC and VERITAS (>400 GeV, empty black squares and black circles, respectively), the Crab flux > 400 GeV (horizontal dashed line), AGILE (> 100 MeV, blue triangle) e) the hardness ratio computed by using the SuperAGILE and ASM data for each day. The dashed Optical and X radiation comes from two different jet regions, each one characterized by its own variability. A possible scenarios is one in which the inner jet region would produce the Xrays and it would be at least partially transparent to the

• ptical radiation. In contrast, the outer region can only produce lower-

frequency emission Donnarumma et al., 2008

Hot News Hot News

These follow the topic of this workshop These follow the topic of this workshop i.e. i.e. Frontier objects in astrophysics Frontier objects in astrophysics

 1. Optically pulsating magnetar  2. V407 Cygni: >100 MeV gamma-ray flare

from Symbiotics Mira

 3. OT in Pegasus, May 2010, and discovery

• f another event from the object 67 years

ago

 4. Possible SGR flare from gamma-ray TeV

emitting binary LSI +61 303

Vulcano Workshop 2010 16

GRB 070610: Flares from a peculiar galactic burst GRB 070610: Flares from a peculiar galactic burst

We recorded over 40 flare episodes Up to I~16, timescales of ~20sec - 7 min Amplitudes over 4 magnitudes

17 Malaga Workshop 2009

GRB 070610 GRB 070610 Gamma-ray Gamma-ray

Optical Galactic gamma-ray burst!

Implications Implications

 A new magnifestation of magnetar activity, becoming

• ne of the few hundred Galactic ones becoming active

in 104 yr. First optical counterpart of SGR.

 The quiescent X-ray luminosity :

Lx < 9 x 1031 (D/5 kpc)2 erg/s is intermediate between transient magnetars

(including SGRs/AXPs):

Lx = (2-4) x 1035 erg/s and dim isolated neutron stars (DINs): Lx = (2-20) x 1030 erg/s

 The missing link between magnetars and DINs ?

18 Malaga Workshop 2009

… … and what this means for and what this means for (optical) observers (optical) observers

 New type of optical variable object (“star”) manifested  Short (~1 to 2 mins) intense (up to mag 7) numerous (~40 in 2

days) flares

 Peak magnitude I ~ 14.8 accessible by a digital CCD camera &

lens

 Expected recurrence – but cannot be predicted  Occurs in Galactic plane  Monitoring of microquasars  Visible variable sky changes! We can see magnetars but also

• bjects up to billions light years far (naked eye GRBs)

19 Vulcano Workshop 2010

The Puzzle of V407 Cygni The Puzzle of V407 Cygni & & gamma-ray emission from gamma-ray emission from symbiotics stars symbiotics stars

20 Vulcano Workshop 2010

V407 Cyg V407 Cyg History History

Discovered
by
Cuno
Hoffmeister
in Discovered
by
Cuno
Hoffmeister
in Sonneberg
in
194 Sonneberg
in
1949 9
as
nova‐like 
as
nova‐like variable variable
(Hoffmeister
1949) 
(Hoffmeister
1949) In
more
detail
first
invesAgated
by In
more
detail
first
invesAgated
by Ludwig
Meinunger
at
the Ludwig
Meinunger
at
the Sonneberg
Observatory
in
1966 Sonneberg
Observatory
in
1966 (Meinunger,
1966) (Meinunger,
1966) Strange
outburst
in
1938
followed Strange
outburst
in
1938
followed by
Mira
like
light
variaAons

with by
Mira
like
light
variaAons

with period
of
745
days period
of
745
days Thermonuclear
event
in
1938? Thermonuclear
event
in
1938?

21 Vulcano Workshop 2010

V407 Cyg V407 Cyg Fact Sheet Fact Sheet



Symbiotic binary harboring a Mira variable, of 745 day pulsation and a possible

• rbital period of 43 years, at a distance of 2.5/3.0 kpc and a reddening of E(B-

V)=0.5/0.6 (Munari et al. 1990).



In addition to a possible previous one in 1936 (when the object was noted for the first time by Hoffmeister 1949), V407 Cyg has been discovered in nova outburst by Nishiyama and Kabashima (2010, CBET # 2199 ) on Mar 10.8 UT.



Spectroscopic confirmation was first provided by Munari et al. (2004, CBET # 2204 )

• n Mar. 13.1 UT. They noted the emergence of the spectrum of a He/N nova that
• verwhelmed the absorption spectrum of the Mira. Numerous and strong emission

lines were observed, which belonged to two distinct groups. The first group, composed by sharp profiles with even narrower central absorptions, originated from the ionized slow wind of the Mira. The second group, characterized by much broader profiles for helium, nitrogen and hydrogen lines , originated from the nova fast expanding ejecta.



Such a scenario was highly reminiscent of the recurrent nova RS Oph. The outburst

• f V407 Cyg has since then been detected also in gamma-rays (ATel #2487) and at

radio wavelengths (ATel #2506, ATel #2511, ATel #2514, ATel #2536), and observed in the infrared (CBET # 2210 ).

22 Vulcano Workshop 2010

Very
bright
outburst
of
symbioAc
star
V407
Cyg.
This
outburst
was
discovered
independently Very
bright
outburst
of
symbioAc
star
V407
Cyg.
This
outburst
was
discovered
independently by
the
team
of
K.
Nishiyama
(Fukuoka,
Japan)
and
F.
Kabashima
(Saga,
Japan),
and
by
T. by
the
team
of
K.
Nishiyama
(Fukuoka,
Japan)
and
F.
Kabashima
(Saga,
Japan),
and
by
T. Kojima
(Tsumagoi,
Agatsuma‐gun,
Gunma‐ken,
Japan).
Nishiyama
and
Kabashima
observed Kojima
(Tsumagoi,
Agatsuma‐gun,
Gunma‐ken,
Japan).
Nishiyama
and
Kabashima
observed the
star
at
an
unfiltered
magnitude
of
6.8
on
2010
March
10.813
(JD
2455266.313)
and the
star
at
an
unfiltered
magnitude
of
6.8
on
2010
March
10.813
(JD
2455266.313)
and magnitude
6.9
on
2010
March
10.814
(2455266.814).
Kojima
observed
the
star
at
around magnitude
6.9
on
2010
March
10.814
(2455266.814).
Kojima
observed
the
star
at
around magnitude
7
on
two
images
taken
using
a
Canon
EOS
40D
(CBET
2199).
The
spectra magnitude
7
on
two
images
taken
using
a
Canon
EOS
40D
(CBET
2199).
The
spectra exhibiAng
spectral
features
clearly
indicaAng
a
classical
nova
of
the
He/N
type
(CBET
2204). exhibiAng
spectral
features
clearly
indicaAng
a
classical
nova
of
the
He/N
type
(CBET
2204).

23 Vulcano Workshop 2010

Recent Optical Light Curve Recent Optical Light Curve of V407Cyg

• f V407Cyg

24 Vulcano Workshop 2010

Gap in optical data! Need for all sky

• ptical monitors

able to detect bright objects

Naked eye limit Meduza Project data

V V 407 407 Cyg as Cyg as a a gamma-ray gamma-ray transient transient

 Fermi LAT Detection of a New Galactic Plane Gamma-ray

Transient in the Cygnus Region: Fermi J2102+4542.

 >100 MeV flux of (1.0 +/- 0.3) x 10^-6 ph cm^-2 s^-1 There is no

previously reported gamma-ray source at this location.

 Within the 95% confidence error circle radius of 0.12 deg is the

symbiotic star V407 Cyg, with a reported optical outburst beginning approximately 2 days earlier (CBET # 2199 ).

 Swift/XRT observations triggered on the optical outburst of

V407 Cyg and performed on March 13th and 15th resulted in 2.4-2.6 sigma (0.3-10 keV) detections of an X-ray source coincident with the position of the star in each of the two 960 sec exposures.

25 Vulcano Workshop 2010

Symbiotic stars as Hard-X-ray emitters (up to 60 keV)

seen by INTEGRAL : RT Cru and CD -57 3057 identified with IGR sources (Masetti et al., 2005) The origin of such hard X-ray emission from these presumably accreting, The origin of such hard X-ray emission from these presumably accreting, non-magnetic white dwarfs (WDs) is a mystery. non-magnetic white dwarfs (WDs) is a mystery. Possible explanations include: 1) Possible explanations include: 1) boundary-layer emission boundary-layer emission from accretion from accretion

• nto a near-Chandrasekhar-mass WD; 2)
• nto a near-Chandrasekhar-mass WD; 2) non-thermal emission from a jet

non-thermal emission from a jet; ; and 3) emission from an and 3) emission from an accretion column accretion column on a WD not previously

• n a WD not previously

recognized as magnetic recognized as magnetic

26 Vulcano Workshop 2010

V407 Cyg Outburst Spectra V407 Cyg Outburst Spectra

The spectral appearance is a highly peculiar one. The spectrum is completely different from those ever recorded for this object and

• ther symbiotic Mira variables in
• utburst. The white dwarf

companion to the Mira variable is experiencing an outburst similar to that of classical novae, and its ejecta are moving in the circumstellar environment already filled by the ionized wind of the Mira (CBET 2204).

27 Vulcano Workshop 2010

Such prominent spectral features will be observable by Gaia satellite BP/RP ultra-low dispersion spectroscope

Comparing Comparing PARI PARI Schmidt Schmidt plate plate vs. vs. Gaia Gibis Simulator Gaia Gibis Simulator

Gaia CU7 Napoli 2010 28

Comparison Gaia BP/RP Low Comparison Gaia BP/RP Low Dispersion Spectra Versus Dispersion Spectra Versus Spectral Low Dispersion Plates Spectral Low Dispersion Plates

plate plate Gaia RP Gaia RP

Gaia CU7 Napoli 2010 29

Scan of a plate Scan of a plate from the from the PARI PARI Case Western Case Western Reserve Univ. Reserve Univ.

• collection. This
• collection. This

plate (#10246) plate (#10246) was taken on was taken on November 17, November 17, 1974 (dec= 1974 (dec= +23.5, RA= +23.5, RA= 4h50m) and is 4h50m) and is part of the Tau part of the Tau Cloud Survey. Cloud Survey. The exposure is The exposure is 72min, 72min, Emulsion Emulsion

PARI USA PARI USA

1983ApJS,51,11 1983ApJS,51,11 7 (Pesch & 7 (Pesch & Sanduleak) Sanduleak)

Case 15834-4-IRAS 02104+6225 Case 15834-4-IRAS 02104+6225

30 Gaia CU7 Napoli 2010

Planetary nebula Planetary nebula

FY Aql and GRB790331 FY Aql and GRB790331

31 Vulcano Workshop 2010

In crowded part of the Milky Way in Aquila. During a standard catalog search of the box, Laros et al. (1985) found that the Mira variable star FY Aql is inside the region. Subsequent studies have found that the Mira star has short-duration flares and a surrounding reflection nebula, while the nebula has subsequently disappeared. Details concerning FY Aql are given in Hartmann & Pogge (1987), Schaefer et al. (1987), Hudec (1987), Schaefer (1990), Schaefer (1991), and Irwin & Zytkow (1994).

FY Aql FY Aql Optical Study Optical Study

Optical study in the field of FY Aql/GRBS Optical study in the field of FY Aql/GRBS 1979 0331 1979 0331 Hudec, Hudec, Rene Rene,

, Bull. Astronomical Institutes of

• Bull. Astronomical Institutes of

Czechoslovakia, 40, no. 4, Aug. 1989, p. 261- Czechoslovakia, 40, no. 4, Aug. 1989, p. 261- 266. 266. Results were presented from an optical Results were presented from an optical investigation of the error box of the gamma- investigation of the error box of the gamma- ray burst source (GRBS) 1979 0331. ray burst source (GRBS) 1979 0331. Consideration is given to the light changes Consideration is given to the light changes and optical behavior of the variable FY and optical behavior of the variable FY

Aql, located inside the box. The results confirm located inside the box. The results confirm that FY Aql is a Mira variable. With that FY Aql is a Mira variable. With short short period flares period flares Mira, Symtiotics system with Mira, Symtiotics system with reflecting nebula indicating possible eruption reflecting nebula indicating possible eruption in the past, positional overlap with GRB in the past, positional overlap with GRB 790331 790331

32 Vulcano Workshop 2010

FY Aql FY Aql

ReflecAve
nebula ReflecAve
nebula Visible
in
Gunn
r
band Visible
in
Gunn
r
band Invisible
in
other
filters Invisible
in
other
filters IndicaAon
for
a
possible IndicaAon
for
a
possible erupAve
episode
in
the erupAve
episode
in
the past past

Hartmann
and
Pogge,
1987 Hartmann
and
Pogge,
1987 Laros
et
al.,
1985,

Hartmann Laros
et
al.,
1985,

Hartmann and
Pogge,
1987) and
Pogge,
1987)

33 Vulcano Workshop 2010

Indication for blue unresolved companion Extended reflective nebula, later disappeared

R A R Aqr qr

The
HST
image,

shows The
HST
image,

shows the
inner
core
of
R
Aqr the
inner
core
of
R
Aqr resolved
into
two
very resolved
into
two
very bright
knots bright
knots The
two
knots,
which The
two
knots,
which appear
as
dark
spots
in appear
as
dark
spots
in the
picture
due
to the
picture
due
to saturaAon,
most
likely saturaAon,
most
likely harbour
the
double harbour
the
double system.
Also
seen
are system.
Also
seen
are filamentary
features filamentary
features emanaAng
from
the
core. emanaAng
from
the
core.

34 Vulcano Workshop 2010

Speculation Speculation

 Symbiotics Miras may undergo a very rare

and very large flares whose relicts can be

• bserved as nebulas around these objects

 These events may be sources of very hard

(gamma-rays > 100 MeV ) transient radiation

Vulcano Workshop 2010 35

CV in Pegasus (May 8,2010) CV in Pegasus (May 8,2010)

 Rare type of DN (WZ Sag type) with very long recurrence time  (67 years) but very large (8 mag or more) amplitudes  Only very few such objects known  Dramatic spectral changes detectable by Gaia  The OT detected on May 8,2010, the historical one Dec 1942

inspectiong ~4000 Sonneberg Observatory Sky Patrol Plates (in 2 days, 1 year~50 plates~5 min, visual inspection), Hudec 2010. 1942 Nov 30 1942 Nov 30 All other times All other times Confirms the importance of Confirms the importance of astronomical plate archives astronomical plate archives

36 Vulcano Workshop 2010

LS I +61 303 LS I +61 303

LS I +61 303: LS I +61 303:

 

High Mass High Mass x-ray binary at a x-ray binary at a distance of 2 kpc distance of 2 kpc

  Optical companion is a

Optical companion is a B0 Ve star B0 Ve star

• f 10.7 mag with a
• f 10.7 mag with a circumstellar disc

circumstellar disc

  Compact object probably a

Compact object probably a neutron neutron star star

 

High eccentricity High eccentricity or the orbit (0.7)

• r the orbit (0.7)

 

Modulation of the emission Modulation of the emission from from radio to x-rays with period radio to x-rays with period 26.5 days 26.5 days attributed to orbital period attributed to orbital period

 

Secondary modulation Secondary modulation of period

• f period 4

4 years years attributed to changes in the Be attributed to changes in the Be star equatorial disc star equatorial disc

0.4 AU 0.4 AU

To observer To observer

37 Vulcano Workshop 2010

LSI +61 303 LSI +61 303 (V615 Cas) (V615 Cas)

 SGR like gamma-ray flare from

the region (position inaccuracy 2 arcmin) of the object (GCN 8209; ATel #1715)

 ? Magnetar in this system?  Small flux decrease in optical

(0.05 mag) ~ 1 day before the flare time (ATel #1765)

 Increased X-ray activity starting

~20 days before flare observed from the region by RXTE (ATel #1730)

Vulcano Workshop 2010 38

LSI +61 303 LSI +61 303

 This is the first manifestation of magnetar-like

activity in a high mass X-ray binary.

 The nature of the compact object in orbit around the

Be companion has been debated and is of major interest to interpret the high energy gamma-ray emission from this system (Mirabel 2006, Science, 312, 1759).

 Based on the above, we conclude LS I +61 303 is

most likely to host a young, highly magnetized pulsar.

Vulcano Workshop 2010 39

Examples of Optical Examples of Optical Monitoring Projects Monitoring Projects

 Suitable for analyses of HE/VHE sources  Many in preparation or operation  4pi of the Sky, ASAS, photographic (Sonneberg

and Ondrejov), HERO, various robotic telescopes, photographic archives, SLOAN, …..

 Many surveys are of deep lim mag but (very)

limited FOV …. Wide Field Monitoring needed

Vulcano Workshop 2010 40

HERO Project HERO Project

project organized by network of small and project organized by network of small and amateur Czech Observatories and Observers amateur Czech Observatories and Observers

Vulcano Workshop 2010 41

List of objects included : 3C 66A, V 347 Aql, FO Aqr, TT Ari, S5 0716+714, 1ES 2344+514, 8C 0149+710, V 709 Cas, V1727 Cyg, 1ES 1959+650,1ES 0647+250, AM Her, HZ Her, Mrk 501, BL Lac, 3C454, 4C 47.08, GK Per, RX J0214.2+5144, S5 0836+710,

Tuorla Blazar Tuorla Blazar Monitoring (wth focus Monitoring (wth focus

• n TeV blazars)
• n TeV blazars)

Vulcano Workshop 2010 42

http://users.utu.fi/kani/1m/

Low-Cost Optical Monitor for Detection of Low-Cost Optical Monitor for Detection of Bright OTs from GRBs and other targets: Bright OTs from GRBs and other targets: Simulations and Experiment Simulations and Experiment

Optical All- Sky Monitor Cost ~ 1.5 k$ Capable to detect bright OTs of GRBs down to mag 10

43 Malaga Workshop 2009

Vulcano Workshop 2010 44

CCD Sky Patrol Test Images Sonneberg lim mag 14-15 (Canon camera + lens)

GRB080319B For ~ 1 minute Brighter in optical light than mag 6

Naked eye visibility at z ~ 0.75

45 Vulcano Workshop 2010

IGR J12349-6434 = RT Cru IGR J12349-6434 = RT Cru

hard X-ray symbiotic star on hard X-ray symbiotic star on

historical

historical

Leiden Franklin

Leiden Franklin Adams Plates Adams Plates INTEGRAL gamma-ray source visible on astronomical plates taken by INTEGRAL gamma-ray source visible on astronomical plates taken by 100 years old optical talescope 100 years old optical talescope 80 years ago 80 years ago Violent (amplitude 3 magnitudes) optical brightness variations identified Violent (amplitude 3 magnitudes) optical brightness variations identified

• n the historical plates
• n the historical plates …

…. Confirmation of classification by Masetti et al. . Confirmation of classification by Masetti et al. We can We can follow the evolution of the source over almost 100 years follow the evolution of the source over almost 100 years

Vulcano Workshop 2010

Conclusions Conclusions

 The HEA/UVE objects in many cases exhibit optical (and

variable) emission

 For many of these sources there is a lack of optical data  The optical data are important for multispectral analyses of the

sources (e.g. TeV, INTEGRAL gamma)

 The rate of bright OTs (incl. recurerent novae et) was severely

underestimated before and only now the WF cameras deliver more numerous detections

 The recent WF monitoring by digital cameras is suitable for

detection of brief OTs in the magnitude range < 12 mag

 There are still new discoveries on visible variable sky such as

flashing magnetars

 Symbiotics Miras may exbibits very rare but very energetic

flares which can be observed in gamma-rays (>100 MeV) and

• ptical

47 Vulcano Workshop 2010

The End The End

48 Vulcano Workshop 2010