Advances in Astronomy

Advances in Astronomy / 2010 / Article
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Robotic Astronomy

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Research Article | Open Access

Volume 2010 |Article ID 594854 | 10 pages | https://doi.org/10.1155/2010/594854

The Role of Ground-Based Robotic Observatories in Satellite Projects

Academic Editor: Alberto J. Castro-Tirado
Received09 Jun 2009
Revised25 Aug 2009
Accepted20 Dec 2009
Published16 Mar 2010

Abstract

We discuss the role of robotic telescopes in satellite projects, as well as related strategies. Most satellite projects in space astrophysics focus on high-energy astrophysics from X-rays to gamma-rays. A large fraction of objects of high-energy astrophysics emit also optical light, which is, in many cases, variable. The observation of these sources at optical wavelengths can provide valuable inputs for multispectral analysis of various categories of celestial high-energy (HE) sources. As the magnitudes of numerous objects are bright and can be hence accessed by robotic ground-based observatories, these observations can contribute to investigations and analyses of HE sources. We discuss in detail this possible contribution, with emphasis on the ESA INTEGRAL mission. In addition to this, there are also satellite projects outside the high-energy astronomy, in which the robotic telescopes can also play an important role. We will illustrate this on the example of the ESA satellite Gaia. In this project, robotic telescopes are expected not only to verify the triggers detected by satellite (such as transients and flares) but also to provide additional (mostly photometric) data for better scientific cases.

1. Introduction

Most satellite projects in space astrophysics focus on high energy astrophysics from X-rays to gamma-rays. A large fraction of objects of high-energy astrophysics emit also optical light, which is, in many cases, variable (Figure 1). The observation of these sources at optical wavelengths can provide valuable inputs for multispectral analysis of various categories of celestial high-energy (HE) sources. As the magnitudes of numerous objects are bright and can be hence accessed by (even small) robotic telescopes, these devices can effectively contribute to investigations and analyses of HE sources.

In addition to this, the robotic telescopes can also play an important role in satellite projects outside high-energy astrophysics. The astrometry mission Gaia of European Space Agency ESA can serve here as an example. As it will be shown later, very common is the situation when we have satellite (e.g., HE) monitoring data covering up to years, but we do not have simultaneous optical data. At the same time, the most important goal is to recognize active states of the sources (flares, high states, etc.) either to trigger the satellite observations, or, alternatively, to be able to concentrate on archival satellite data for those periods. In this aspect, robotic observatories can effectively contribute.

2. The Role of Monitors

Some types of astrophysical objects (e.g., blazars, cataclysmic variables, gamma-ray bursters, flare stars, etc.) exhibit rare flares for which satellite observations are important. These events cannot be monitored by satellites themselves in most cases. These events can be effectively monitored by ground based robotic telescopes (RT) generating ToO (Target of Opportunity) triggers for satellites with ToO regime.

The monitors, in contrast to alert telescopes, can deliver optical photometric data for objects prior and during the active/flaring states—wide-field (WF) coverage is important to cover as many sources as possible. There is a scientifically justified need to have this mode in robotic (i.e., autonomous remotely controlled) telescopes. RT with reasonably large field of view (FOV), performing regular sky surveys, or with an attached WF camera, can serve as a monitoring device. In some cases, even post-flare monitoring is important as shown by magnetar candidate GRB070610 optical flares [1] in order to ( ) detect the optical flares and ( ) detect possible recurrence (this is a very difficult task, but important one, which can be performed only by robotic instruments as the recurrence cannot be predicted).

3. The HE Sources as Optical Emitters

The HE sources belong to both galactic as well as extragalactic sources. In the following subsections we will very briefly discuss both groups.

3.1. Galactic HE Sources

There are numerous categories of galactic HE sources, most important ones are listed below:

(1)Cataclysmic Variables (CVs) and related objects, example: GK Per,(2)Low Mass X-ray Binaries (LMXRB), example: HZ Her = Her X-1,(3)High Mass X-ray Binaries (HMXRB), example: Cyg X-1,(4)X-ray transients,(5)New types of sources.

The fact that there are numerous CVs among the gamma-ray sources observed by the ESA INTEGRAL satellite (perhaps up to 10% of all INTEGRAL gamma-ray sources) represent one of interesting new findings over the last few years. Moreover, few symbiotic stars (SSs) were also identified with INTEGRAL gamma-ray sources.

3.1.1. Are the Optically Variable Galactic HE Sources “Variable Stars”?

As many of the HE sources do have optical variable emission, a natural question arises, what is the link between these sources and classical variable stars (VS).

(1)Yes, some are X-ray and gamma-ray loud cataclysmic variables and symbiotic stars (SS) can serve as examples.(2)Some of LMXRB, HMXRB are VS of “non-classical categories”.(3)Some are newly detected VS.(4)Some are not VS such as the new category of galactic gamma-ray bursts (GRBs).(5)The dominant role of CVs is obvious: The contribution of CVs to galactic X-ray background may be greater than assumed before, based on INTEGRAL results in hard X-rays (IBIS experiment).
3.2. Extragalactic HE Sources

Numerous celestial HE sources belong to the category of extragalactic sources; the most important types are listed below:

(1)AGN,(2)Blazars,(3)Optical Afterglows and Optical Transients of Gamma-Ray Bursts (GRBs),(4)SNe,(5)LBV (Luminous Blue Variables in external galaxies). They are worth study as they can at some active states mimic the light behaviour of optical afterglows of GRBs.

Several examples of the blazars detected in gamma-rays by the INTEGRAL satellite are given and discussed later in this paper.

4. Modes of Observations

There are various modes of optical observations required for the HE sources. The situation is very complex, as the sources belong to various categories.

Satellite Campaigns
One of the most important modes of supporting optical ground-based observations is the response to satellite observing campaigns. While the satellite observation itself usually lasts for several days, the whole observing campaign lasts typically for weeks, as also the time interval before and after the satellite observation needs to be covered. Dense coverage during the satellite observation is required, with less dense coverage before and after. Magnitudes of the targets are typically 12–18 but occasionally can go deeper. Example: satellite campaigns organized by blazar observers.
In addition to that, planned observations (mostly known in advance) of optically variable sources by satellites can be supplemented by optical ground based observations, with similar requirements as described above. Example: simultaneous optical observations for targets approved for Newton, Chandra, INTEGRAL.

Monitoring for Triggering Satellite (ToO—Target of Opportunity) Observations
They belong to another important type of optical observations of HE sources. In most cases, moderate samp1ing of 1 point/day is enough. Magnitudes are typically 12–18. Example: ToO proposal on blazars within INTEGRAL project. Here, the blazars included in the approved list are to be optically monitored for possible brightening. Again, about 1 photometric point/day is acceptable for most of the sources.

Providing Optical Data for Non-Triggered Satellite Observations
They represent another category (e.g., providing optical monitoring data for the time span of INTEGRAL operation, i.e., 2002–2012). Typically 1 point/day (or even less) is enough. Magnitudes of most of the objects are typically within the range 10–18. This type of observations allows to compare behaviour of gamma-ray sources at various energies and is hence physically important as from such comparison physical interpretations and conclusions may be drawn. Example: Ondrejov D50 RT long-term monitoring of INTEGRAL CVs and blazars.

Alert Followup Observations
They represent another important type. They need fast response, better (but not necessarily) automated. However, even a site with non automated instrumentation has chance due to observational/weather constraints. Mostly Gamma-Ray Bursts (GRBs) belong to the group of objects observed this way, but occasionally various types of other flaring and transient targets may be added. Expected magnitudes are 6–22 but in some cases (optically dim GRBs) even fainter. With the ESA Gaia satellite, we expect another (Gaia project related) type of alerts, which will point on suspicious (mostly flaring) objects detected within Gaia. As the Gaia itself will have limited ability to confirm the reality of these objects, in most cases the final confirmation and further analyses of Gaia alert triggers will rely on ground based (preferably robotic) observers. Example: GRB followup.

Verifying Suggested Identifications
They represent another type of job where robotic observatories may contribute. Typical magnitudes are 10–20. The preferred response is within days or a week. Photometry both with good sampling as well as moderate sampling, photometry with filters, spectroscopy (including low dispersion), are required. Example: confirmation of INTEGRAL CV candidates revealed by optical spectroscopy.

Optical Supplementary Analyses
Optical supplementary analyses of HE sources (for complex multispectral analyses) may also add valuable optical data for understanding the physics of the sources. The typical magnitudes are 10–20. Again, photometry both with good sampling as well as moderate sampling, photometry with filters, and spectroscopy (including low dispersion) are required. Example: Investigation of gamma-ray loud blazars in optical light.

5. Examples of Ground-Based Observations

5.1. INTEGRAL Cataclysmic Variables

The ESA INTEGRAL satellite [2], launched in 2002 and expected to operate at least until 2012, with its 4 onboard telescopes for analyses of gamma-ray sources simultaneously in gamma-ray, X-rays, and (for brighter objects) optical band, is suitable for: (a) detection of the populations of CVs and symbiotics with the hardest X-ray spectra, (b) simultaneous observations in the optical and hard X-ray regions, and (c) long-term observations with Optical Monitoring Camera (OMC)—including a search for rapid variations in observing series during science window (OMC observations also for systems bellow the detection limit in hard X-rays).

In total, 32 CVs were detected (surprise, more than expected, almost 10% of INTEGRAL detections, see Table 1). 28 CVs were seen by IBIS [68]—based on correlation of IBIS data and Downes CV catalogue [9]. 4 are CV candidates revealed by optical spectroscopy of IGR sources [10]—new CVs, not in Downes catalogue. They are mainly magnetic systems: 22 confirmed or propable intermediate polars (IPs), 3 polars, 2 dwarf novae, 4 probable magnetic CVs, 1 unknown. Periods: vast majority  hr, that is, above the period gap (only one 3 h). 5 long period systems with  hr. Some statistics: Intermediate polars represent only 2% of the catalogued CVs, but they dominate the group of CVs seen by IBIS. More such detections and new identifications can be hence expected. Many CVs covered remain unobservable by IBIS, but new have been discovered. IBIS tends to detect IPs and asynchronous polars: in hard X-rays, these objects seem to be more luminous (up to the factor of 10) than synchronous polars (but detection of more CVs needed for better statistics). A few examples are listed and discussed below.


Detected CVs
GCVS NameRA (2000)DEC (2000)Object Type

IGR J00234 6141 00:22:57.63 61:41:07.8dq
V709 Cas 00:28:48.84 59:17:22.3dq
XY Ari 02:56:08.10 19:26:34.0dq
GK Per 03:31:12.01 43:54:15.4na/dq
V1062 Tau 05:02:27.47 24:45:23.4dq
TV Col 05:29:25.52 32:49:04.0dq
IGR J05346 5759 05:34:50.60 58:01:40.7vy:
BY Cam 05:42:48.77 60:51:31.5am
MU Cam 06:25:16.18 73:34:39.2dq
IGR J08390 4833 08:38:49.11 48:31:24.7cv
XSS J12270 4859 12:27:58.90 48:53:44.0dq
V834 Cen 14:09:07.30 45:17:16.2am
IGR J14536 5522 14:53:41.06 55:21:38.7dq
IGR J15094 6649 15:09:26.01 66:49:23.3dq
NY Lup 15:48:14.59 45:28:40.5dq
IGR J16167 4957 16:16:37.20 49:58:47.5dq:
IGR J16500 3307 16:49:55.64 33:07:02.0dq
V2400 Oph 17:12:36.43 24:14:44.7dq
IGR J17195 4100 17:19:35.60 41:00:54.5dq:
IGR J17303 0601 17:30:21.90 05:59:32.1dq
V2487 Oph 17:31:59.80 19:13:56.0na
AM Her18:16:13.33 49:52:04.3am
IGR J18173 2509 18:17:22.25 25:08:42.9cv
V1223 Sgr 18:55:02.31 31:09:49.6dq
IGR J1 9267 1325 19 26 27.03 13 22 03.2cv
V1432 Aql 19:40:11.42 10:25:25.8am
V2306 CYg 19:58:14.48 32:32:42.2dq
V2069 CYg 21:23:44.84 42:18:01.8dq:
IGR J21335 5105 21:33:43.65 51:07:24.5dq
SS CYg 21:42:42.80 43:35:09.9ugss
FO Aqr 22:17:55.39 08:21:03.8dq
AO Psc 22:55:17.99 03:10:40.0dq

V Cen
The optical light curve of V834 Cen during the lifetime of INTEGRAL shows active and inactive states. V834 Cen is a polar of AM Her class. This polar was probably detected by IBIS since it was in high (active, both optical and gamma-ray) state. This may explain why some CVs have been detected by IBIS and some not. Optical monitoring of sources is important as it can indicate active intervals when the object is expected to be active also in gamma-rays. However, comparing optical and gamma-ray activity is difficult in most cases due to lack of optical data. This is definitely a goal for robotic telescopes (example of monitoring of GK Per is shown in Figure 6).

V Sgr
This object is an intermediate polar and represents the most significantly detected CV in the INTEGRAL IBIS survey, with a significance of 38 sigma in the 20–40 keV final mosaic (Figures 2, 3, and 4, Table 2). Accretion via disk, bright X-ray source (4U 1849–31). Orbital period:  h [11, 12]. Rotational period of the white dwarf:  sec [12]. Beat period (combined effect of and ):  sec [13].
Prominent long-term brightness variations: (i) outburst with a duration of 6 hr and amplitude 1 mag [14], (ii) episodes of deep low state (decrease by several magnitudes) [15]. The object exhibits high-energy flaring activity: seen by IBIS (flare lasting for 3.5 hrs during revolution 61 (MJD 52743), peak flux 3 times of the average [6]. Analogous flares were seen also in optical (but at other times) by ground-based instrumentation (duration 624 hrs [14]). This confirms the importance of OMC instrument onboard INTEGRAL: even with lim mag 15, it can provide valuable optical simultaneous data to gamma-ray observations.
Similar flares are known also for another IPs in optical, but not in soft gamma rays: Example TV Col [3], where 12 optical flares have been observed so far, five of them on archival southern sky patrol plates from the Bamberg Observatory (Figure 5). TV Col is an intermediate polar and the optical counterpart of the X-ray source 2A0526-328 [16]. TV Col is the first cataclysmic variable (CV) discovered through its X-ray emission. Recently TV Col was detected by INTEGRAL IBIS as a hard X-ray source [8]. Physics of the outbursts in IPs is either disk instability or an increase in mass transfer from the secondary.


JD (24 )Exp. TimeFlux (15–25) keVFlux (25–40) keVFlux (40–60) keVFlux (60–80) keV
[  erg  ][  erg  ][  erg  ][  erg  ]

52 710.38 52 752.01109.2161.00 14.5057.90 4.88 4.93 6.26
52 917.17 52 926.84151.1112.00 11.3051.10 4.1921.30 4.24 5.48
53 082.07 53 119.10228.1127.00 8.9050.00 3.2823.10 3.4810.00 4.54
53 267.41 53 305.97134.5126.00 12.5055.40 4.4625.40 4.7527.70 6.23
53 440.61 53 479.8190.9155.00 15.2061.30 5.5324.10 5.85 7.69
53 602.80 53 672.88409.6 7.1731.80 2.65 2.82 3.78
53 781.06 53 809.24282.1132.00 10.0048.50 3.5013.90 3.56 4.69
52 710.38 53 809.251405.5103.00 3.9046.40 1.42 15.10 1.48 12.30 1.97

5.2. INTEGRAL Blazars

From the extragalactic HE sources, blazars belong to the most important and also optically violently variable objects. In Table 3, we list a few examples of blazars analyzed with INTEGRAL observations.


SourceRA DEC Gal coord.ztype

lES 0647+25006 50 46.6 25 03 00190.28310.9960.2030BL Lac
PKS 0823 22308 26 01.5729 22 30 27.204243.9908.9300.9100Possible Q
lES 2344+51423 47 04.919 51 42 17.87112.892 9.9080.0440BL Lac
8C 0149+71001 53 25.8511 71 15 06.463127.9208.9830.0220Q
4C 47.0803 03 35.2422 47 16 16.276144.986 9.8630.4750BL Lac
87GB 02109+513001 03 28.1 43 22 59BL Lac
BL Lac22 02 43.2914 42 16 39.98092.590 10.4410.0688BL Lac
S5 0716+71407 21 53.4485 71 20 36 363143.98128.0180.3000BL Lac
S5 0836+71008 41 24.3653 70 53 42.173143.54134.4262.1720Q
3C 454.322 53 57.7479 16 08 53.56186.111 38.1840.8590Q
3C 27912 56 11.1665 05 47 21.525305,10457.0620.5362Q
3C 2732 29 06.6997 02 03 08.598 11.0104.3800.1583Q
PKS1830 21118 33 39.888 21 03 39.7712.166 5.7122.5070Q
Mrk42111 04 27.3139 38 12 31.799179.83265.0320.0300BL Lac
J1656.3 330216 56 19.2 33 01 48350.6046.361?
IGR J22517+221822 51 53.498 22 17 37.2989.690 32.7503.6680Q
PKS0537 44105 38 43.5 44 05 05250.078 31.1100.8960BL Lac
3C 66A02 22 39.6115 43 02 07.799140.143 16.7670.4440Blazar
Mrk 50116 53 52.2167 39 45 36.60963.60038.8590.0336BL Lac
1ES2344+51423 47 04.919 51 42 17.87112.892 9.9080.0440BL Lac
1ES 1959+65019 59 59.8521 65 08 54 65398.00317.6700.0480Blazar

ES +
This blazar is a gamma-ray loud variable object visible by IBIS in 2006 only, invisible in total mosaics and/or other periods. The optical light curve available for this light curve confirms the relation of active gamma-ray and active opticalstate (Figures 7 and 8).

C A
This blazar is visible by IBIS gamma-ray imager onboard INTEGRAL only during the optical flare shown below and is invisible other times (Figures 9 and 10). This confirms the importance of monitoring of the object in the optical light.

5.3. Identification and Classification of HE Sources

The RT can also serve as a effective tool in identification and classification of HE sources by optical monitoring and consequent detailed optical analyses of the error box content. Many of the HE are optically variable and hence can be identified (and classified) by their optical variability (Figure 11).

5.4. Poorly Understood Objects

In addition to the main types of HE objects described above, occasionally also objects worth study of another category appear. The variable objects at positions of Ultra High-Energy (UHE) sources can serve as an example, for example, the puzzling poorly investigated variable star at position of UHE source, namely the variable M6 star V347 Aql, with coordinates J2000.0 ICRS position of RA 19 h 08 m 01.3 s, , and magnitude  mag. The star is within the error box of the new VHE (very high energy) source HESS J1908+063. The nature of this star (which is also an IRAS source) is unknown, previous possible classifications were a possible T Tauri star, or an oxygen rich irregular variable star.

The light curve is unknown, albeit the object magnitude amounts to B 11, that is, the star is a good target for small robotic observatories (Figure 12).

5.5. New Types of Optically Variable Objects

There are also newly detected types of optically variable HE sources. The optical counterpart of GRB070610/SWIFT J195509 261406 may serve as an example [1, 17]. The basic parameters of this GRB are as follows: detected on 10 June 2007 20:52:26 UT by Swift/BAT as a normal burst [18],  s, Photon index 1.76 0.25, Fluence (2.4 0.4)  erg/ [19], XRT detected an X-ray counterpart 3100 s later [20] with a column density consistent with the Galactic. Pagani et al. [21] reported the detection of a variable optical counterpart, de Ugarte Postigo et al. [22] confirmed the detection with observations from the 1.5 m OSN. Kann et al. [23] suggested a Galactic origin, based on unusual flaring activity and location near the galactic plane: . About 40 optical flares peaking at up to mag 14 as shown on Figure 13. The emission between flares slowly decreased until it disappeared with no detectable quiescent source.

6. Supplementary Optical Data for Non-HE Satellites

Another important role of robotic telescopes is in satellite projects outside high-energy astrophysics. The ESA Gaia project may serve as an example. Albeit its main goal is the ultra precise astrometry, Gaia will monitor all celestial objects down to magnitude 20 over a 5 years’ time period. However, the photometric sampling will not be optimal; hence the supplementary observations provided by ground-based robotic telescopes are expected to provide a valuable contribution. The main goal of these supplementary observations are as follows: ( ) confirm triggers (e.g., optical transients, flares, brightenings, etc.) detected by Gaia satellite and ( ) provide additional photometric data with more dense sampling than provided by the satellite. The HE objects such as LMXRB, HMXRB, and Optical Afterglows and Optical Transients of GRBs can serve here as an example, together with various types of cataclysmic variables including SNe.

The peculiarity of ESA Gaia, where a substantial fraction of data will be as ultra-low dispersion spectra, raises a question about the role of focal devices with dispersive elements, that is, on a spectral alternative. This is fully scientifically justified, as the spectral type of Cepheids, Miras & Peculiar Stars is known to change significantly with time. For example, all classical Cepheids definitely vary their spectral types. At maximum, they all have types around F5–F8. At minimum, the longer the period, the later is the spectral type (to K2) [24]. The long-term behaviour of spectral types of various variable celestial objects (so far only poorly investigated) may be a significant goal not only for ESA Gaia, but also for robotic ground-based optical telescopes equipped with corresponding dispersive elements.

7. Supplementary Optical Data for CTA

The CTA (Cherenkov Telescope Array), albeit not being a satellite, is in many aspects similar to satellite projects (see also the CTA effort at INTEGRAL Science Data Centre ISDC). There is a need for robotic monitoring of VHE (TeV) sources, and alert system for TeV flaring triggers, for example, 1ES1959 650 (TeV blazar at ). There was an essential progress in Cherenkov telescopes over past years, and nowadays these deliver data analogous to what is known from other energy pass bands (i.e., images and light curves). We propose to implement in Cerenkov systems analogous alert system as those currently used on satellites (i.e., rapid alerts sent to optical and radio observers). But also the opposite way may be essential, as the optical robotic telescopes can monitor TeV sources and report detected flares and active periods to Cherenkov teams.

8. Conclusions

The HE objects in many cases exhibit optical (and mostly variable emission) accessible in some cases even by small robotic observatories. For many of these sources there is a lack of optical data. The optical data provided by automated ground-based optical telescopes are important for multispectral analyses of the sources, contributing of better understanding of related physical processes. Even small apertures may contribute as some sources are brighter than magnitude 12. In addition to that, robotic telescopes may play an important role also in satellite projects outside HE astrophysics, as shown on the example of the ESA Gaia, namely as devices confirming the satellite triggers, as well as delivering additional well sampled photometric data for particular objects.

Acknowledgments

The analyses of HE sources by the ESA INTEGRAL satellite were supported by ESA PECS project no. 98023, and in optical by grant 205/08/1207 provided by Grant Agency of the Czech Republic. The investigation of high-energy sources and cataclysmic variables by the ESA Gaia satellite is supported by the ESA PECS Project no. 98058. The analyses of GRBs in optical light including robotic telescopes are supported by the grant of the Grant Agency of the Czech Republic, 102/09/0997. The investigations of the Bamberg Observatory archival plates are supported by DAAD-AVCR project DAAD-25-CZ4/08 and the analyses of PARI plates by MSMT KONTAKT ME09027.

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Copyright © 2010 R. Hudec. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

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