PLAN FOR VLBI OBSERVATIONS OF CLOSE APPROACHES OF JUPITER TO COMPACT EXTRAGALACTIC RADIO SOURCES IN 2014-2016

A. GIRDIUK, O. TITOV

Saint-Petersburg State University

Universitetsky prospect 28, Petrodvorets, 198504, Saint-Petersburg, Russia

e-mail: girduik@ipa.nw.ru

Geoscience Australia

PO Box 378, Canberra, ACT 2601, Australia

e-mail: Oleg.Titov@ga.gov.au

ABSTRACT. Very Long Baseline Interferometry is capable of measuring the gravitational delay caused by the Sun and planet gravitational fields. The post-Newtonian parameter is now estimated with accuracy of using a global set of VLBI data from 1979 to present (Lambert, Gontier, 2009), and by the Cassini spacecraft (Bertotti et. al, 2003). Unfortunately, VLBI observations in S- and X-bands very close to the Solar limb (less than 2-3 degrees) are not possible due to the strong turbulence in the Solar corona. Instead, the close approach of big planets to the line of sight of the reference quasars could be also used for testing of the general relativity theory with VLBI. Jupiter is the most appropriate among the big planets due to its large mass and relatively fast apparent motion across the celestial sphere. Six close approaches of Jupiter with quasars in 2014-2016 were found using the DE405/LE405 ephemerides, including one occultation in 2016. We have formed tables of visibility for all six events for VLBI radio telescopes participating in regular IVS programs. Expected magnitudes of the relativistic effects to be measured during these events are discussed in this paper.

1. USING VLBI OBSERVATIONS FOR TESTING GENERAL RELATIVITY

Close approaches of the Sun and Jupiter to the apparent positions of compact extragalactic radio sources are used to estimate the PPN parameter by the geodetic VLBI technique. A first attempt to test the general relativity theory using the close pass of Jupiter to quasar 0201+113 has been done in 1988 (Schuh et al., 1988) at the angular distance of 3.5. A more famous experiment was arranged on 8 Sep 2002 (Fomalont & Kopeikin, 2003) when Jupiter approached quasar J0842+1835 at the angular distance of 3.7. Variations of the relative separation on the sky between this quasar and a reference radio source were measured by the VLBA network and the Effelsberg 100-meter radio telescope. Another experiment was done on 18 November, 2008 as a part of the session OHIG60 arranged by the International VLBI Service. During this session Jupiter approached quasar 1922-224 at an angular distance of 1.2. Four VLBI stations observed this event for about 12 hours.

2. ESTIMATION OF THE PPN-PARAMETER FROM THE VLBI OBSERVATIONS

Besides three classical tests, the fourth test of general relativity - the delay of a signal propagating in the gravitational field, has been proposed by Shapiro (1964) and known as the Shapiro delay. The difference between two Shapiro delays as measured with two radio telescopes gives a gravitational delay which must be considered at the standard reduction of the high-precision geodetic VLBI data. The IERS Conventions 2010 (Petit and Luzum, 2010) comprises the ’consensus’ formula for the gravitational delay which is valid for the most cases unless a distant quasar and a deflecting body are too close. This formula is presented as follows

(1) |

where - the PPN-parameter of general relativity (Will, 1993), - the gravitational constant, - the mass of gravitational body, - speed of light, - the barycentric unit vector towards the radio source and - the vector between gravitatiting body’s center of mass and -th telescope (see i.e. Kopeikin (1990), Hellings and Shahid-Saless (1991), Klioner (1991) for more details).

An expression that links the gravitational delay and the formula for the light deflection angle (Einstain, 1916) yet to be developed. To obtain it we have expanded the gravitational delay using the Taylor times series on . Finally, the main terms of this expansion are given by

(2) |

where vectors , , and angles , , and are shown on Fig. 1 (Turyshev, 2009).

Surprisingly, we found the first term in (2) is equal to the term including the PPN parameter at the geometric delay, but with opposite sign. Keeping in mind that () the formula for the total group delay recommended by the IAU (Eubanks, 1991), Petit and Luzum (2010):

(3) |

where is the resultant contribution of the general relativity (GR) effects to the , includes two relavistic terms which cancel each other out. Then, may be written as follows

(4) |

or, from (2) and (4)

(5) |

Given that in general relativity, and ingoring for the sake of simplicity

(6) |

For the approximation of small angles (if ), (6) comes down to

(7) |

where is the linear impact parameter. It is now easily to note that the term (7) corresponds to the formula of the light deflection developed by Einstein in 1916:

(8) |

as follows

(9) |

Formula (9) proves that in the first approximation the deflection angle (8) as measured with the geodetic VLBI is independent on a baseline length. The factor is individual for each baseline Fig.2, therefore, implication of the angle in (9) is important.

Fig. 2 displays the dependence of the factor on the calculation of the deflection angle in the plane of equatorial coordinates (). The left plot shows the angle

(10) |

for four individual baselines (from the OHIG60 experiment on 18 November, 2008), where is calculated by (7). The right plot shows the angle as

(11) |

All four individual curves shown on the left plot are merging to one common pathway on the right plot. Thus, it proves that the angle must be taken into account for proper conversion from to and vice versa as (9) and (11). This is also true for an arbitrary angle in (6).

3.FUTURE EVENTS AND THEIR SCHEDULING

N | quasar | date | Flux, mJy | , mas | small terms, pks, for b=6000 km | |
---|---|---|---|---|---|---|

1 | 0846+184 | 28.08.2014 | 45 | ? | 6.0 | 8.5 |

2 | 0918+167 | 09.02.2015 | 30 | ? | 12.8 | 39.1 |

3 | 0912+171 | 24.05.2015 | 39 | ? | 7.7 | 14.2 |

4 | 0920+168 | 08.06.2015 | 37 | ? | 7.8 | 14.8 |

5 | 1109+070 | 26.03.2016 | 26 | 14.5 | 50.1 | |

6 | 1101+077 | 09.04.2016 | 20(8) | 16(46) | 142(503) |

angular distance | 170 | 148 | 126 | 104 | 83 | 64 | 48 | 41 | 46 | 61 | 79 | 100 | 121 | 143 | 166 |
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|

station/UT | 4 | 5 | 6 | 7 | 8 | 9 | 10 | 11 | 12 | 13 | 14 | 15 | 16 | 17 | 18 |

Badary | + | + | + | + | + | + | + | + | + | + | + | + | + | ||

Svetloe, Zelenchuk | + | + | + | + | + | + | + | + | + | + | + | + | |||

Medicina, Hartrao, Yebes | + | + | + | + | + | + | + | + | + | + | |||||

Kokee, MN-VLBA, Seshan25 | + | + | + | + | + | ||||||||||

FD-LA-KP-OV-BR-VLBA, Pietown | + | + | + | + | |||||||||||

SC-HN-NL-VLBA | + | + | + | + | |||||||||||

Parkes, Tsukub32 | + | + | + | + | + | + | + | + |

Six close approaches of Jupiter to quasars will happen in 2014-2016 including one occultation. Table 1 shows names of quasars, dates of event, impact parameters , flux densities (X-band), the maximum angles of the light deflection for the major term and the contributions of the minor terms in (2) for baseline length of km and . A total occultation of the Jupiter by the quasar 1101+077 will happen on 9 April, 2016. Therefore, the numbers for the minimum angle and the angle at the limb of Jupiter are shown separately for that event. Flux densities of four quasars from Table 1 are not available presently and should be measured as soon as possible.

Table 2 presents a visibility chart for several VLBI radio telescopes for the event on 8 June, 2015. This event will last than more ten hours (when the angular distance between objects is less then ). The sign ’+’ notes the hour when both objects will be above the level of horizon for a particular VLBI station. Due to very weak flux for the quasars in Table 1, we have preselected only large size radio telescopes to ensure a reasonal integration time (300 seconds). Thus, many small VLBI radio telescopes were discarded from Table 1 after repeated calculations of the integration time.

4. PLAN FOR VLBI OBSERVATIONS

The maximum deflection angle for the list of close approaches in Table 1 is 16 mas, or equivalent to the time delay of about 1600 pks for a baseline of 6000 km length. When the current accuracy of a single group delay as measured by VLBI is about 30 pks, the relative accuracy of would reach . Conservatively, it would be possible to evaluate the parameter with accuracy for a single VLBI experiment, if a substantial number of VLBI group delays is collected. In addition, it may be possible for one to prove existence of the minor terms from the last column of Table 1 for the two last approaches. It is necessary to organize as many large radio telescopes as possible to maximize a potential amount of observations. Therefore, we are planning to submit proposals for the large available networks (IVS, VLBA, LBA) to observe these rare events.

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