From: Michael Lindqvist <michael.lindqvist_at_email.protected>
Date: Mon, 26 Sep 2016 12:54:52 +0000

Dear all,

Please be reminded about the 1st October Deadline for EVN proposals.


Best regards,
Michael Lindqvist
EVN PC Chair



From: Michael Lindqvist <michael.lindqvist_at_email.protected>
Date: Monday 5 September 2016 14:04
To: "vlbiobs_at_email.protected>
Subject: EVN Call for Proposals - 1st October 2016 Deadline

European VLBI Network
Call for Proposals
Deadline 1st October 2016
[cid:image001.png_at_email.protected]

Introduction

The European VLBI (Very Long Baseline Interferometry) Network (EVN, http://www.evlbi.org/) is a network of radio telescopes in Europe, Asia, South Africa and North America, which allows imaging at radio wavelengths with millarcsecond resolution (from 0.001'' to 0.1'') using the VLBI technique. Wavelengths covered are from 0.7 cm (43 GHz) to 90 cm (345 MHz).

The EVN facility is open to all astronomers. Use of the Network by astronomers not specialised in the VLBI technique is encouraged.

The Joint Institute for VLBI ERIC (JIVE) in the Netherlands can provide support and advice on proposal preparation, scheduling, correlation and analysis (http://www.jive.eu/evn-user-support-jive).

The next proposal deadline is October 1st 2016. Further details and web links to the EVN can be found in the attached detailed call for proposals. The detailed call for proposals can also be found here:
http://www.oso.chalmers.se/evn/call.txt<http://www.oso.chalmers.se/evn/calloct16.txt>


VLBI science

VLBI continuum observations generally observe high brightness temperature radio emission from synchrotron or gyro-synchrotron processes with thermal emission perhaps detectable on short baselines. Radio spectral lines are observable in maser emission (mainly OH, H2O, CH3OH, and SiO) and in absorption against bright continuum sources (mainly in HI and OH).

VLBI observations with full-Stokes correlation allow investigation of polarization structure within your continuum or spectral-line sources. This in turn would allow detection and estimation of magnetic fields and ionised gas densities via Zeeman splitting, Faraday rotation, and Faraday depolarisation mechanisms.

VLBI has the extreme angular resolution to follow changes in source structure on timescales of hours (for stars), months (for many Galactic objects), and years (for many high-redshift systems).

Absolute and relative astrometry of compact radio structure is possible at the (sub)milliarsecond level, which for Galactic objects may allow the measurement of both parallax and proper motion to be made.

A selection of recent highlights is presented here: http://www.jive.eu/jivewiki/doku.php?id=evn:evn_science

A selection of refereed EVN publications during 2016 is presented here: http://www.jive.eu/jivewiki/doku.php?id=evn:evn_publications

Additional information

Further information on EVN observations, and guidelines for proposal submission are available at:
http://www.jive.eu/jivewiki/doku.php?id=evn:guidelines

The EVN User Guide (http://www.evlbi.org/user_guide/user_guide.html) describes the network and provides general information on its capabilities.

Apologies if you have already received this message and for any cross-posting.

Best regards,
Michael Lindqvist
EVN PC Chair


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Michael Lindqvist

Onsala Space Observatory

S-439 92 Onsala

Sweden

Phone: +46-31-7725508

Fax: +46-31-7725590

E-mail: Michael.Lindqvist_at_email.protectedalmers.se<mailto:Michael.Lindqvist_at_email.protected>

WWW: http://www.chalmers.se/rss

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Received on 2016-09-26 22:55:52