Recent news and science highlights from e-MERLIN, MERLIN and VLBI
Announcement of e-MERLIN data school and early science meeting
The e-MERLIN instrument is a high-resolution radio interferometer, capable of routine sub-arcsecond resolution imaging at centimetre wavelengths to sensitivity levels of a few microJy. Observations are competitively allocated by the Panel for the Allocation of Telescope Time, with a substantial proportion of time in the first few years being reserved for large Legacy Programmes. The science programme is wide-ranging and includes the study of the history of star-formation and black hole growth in galaxies, the physical processes which govern the formation of stars, the modes of activity in nearby galaxies, and the energetic processes in relativistic outflows from jets generated by black holes and compact objects.
e-MERLIN has now been in full operational mode for some months, and a meeting will be held in Manchester from 10-11 April 2014 to discuss early science, both from the Legacy projects and from PATT observations from Cycle 0 and the early part of the Cycle 1 allocations. Prior to that, on 20-21 January, there will be a two-day data school, the aim of which will be to help those unfamiliar with the techniques of radio interferometry to reduce e-MERLIN data, including the use of existing analysis pipelines provided by the observatory, in time to present results at the early science meeting.
Please see Meeting webpages for registration details and more information
Deadline : Midnight (23:59 GMT) 17th June 2013
The second open round for e-MERLIN proposals is planned for 2013, with observations scheduled for September 2013 onwards.
Mysterious hot spots observed in a cool red supergiant
25th April 2013
Astronomers have released a new image of the outer atmosphere of Betelgeuse one of the nearest red supergiants to Earth revealing the detailed structure of the matter being thrown off the star.
The new image, taken by the e-MERLIN radio telescope array operated from the Jodrell Bank Observatory in Cheshire, also shows regions of surprisingly hot gas in the star?s outer atmosphere and a cooler arc of gas weighing almost as much as the Earth.
K-band status and upgrades:
Work is progressing on upgrading the eMERLIN K band receivers by replacing the low noise amplifiers (LNAs) with a new MMIC design. Current tests indicate that the new LNAs will deliver a more uniform and significantly lower system temperature across the band from about 19.9 GHz to 26 GHz while providing the full 2GHz per polarization eMERLIN bandwidth.
Initial telescope tests are currently expected towards the end of summer 2013, with the full system expected to be deployed on all e-MERLIN telescopes and available for Cycle-2 observations.
e-MERLIN reveals the structure of a new 'superluminal transient' source in M82
Recent observations using the newly available e-MERLIN telescope have revealed the resolved structure of 'superluminal transient' radio source in M82. Results from these new observations, which have been obtained for the LeMMINGs e-MERLIN legacy project have recently been presented at a large international conference in Bordeaux, France.
The left image shows a high resolution Global VLBI image at 5GHz of the transient source in M82. The right-hand image show the same source observed with e-MERLIN in 2012. Whilst at lower resolution the sensitivity and imaging quality of e-MERLIN allows this source to be resolved in an east-west direction confirming the earlier MERLIN proper motion estimates of its expansion and the VLBI imaging. These e-MERLIN (and VLBI) observations are part of ongoing research under the e-MERLIN legacy project, LeMMINGs.
The boiling face of Betelgeuse
e-MERLIN has resolved fine details on the face of Betelgeuse. These are the highest-resolution images at cm wavelengths which show the full extent of the radiio photosphere, 25 AU (125 milli-arcsec) in radius, 6 times the optical photosphere. The sensitivity afforded by 500 MHz bandwidth, centred on 5.75 GHz (5.2 cm), reveals an additional arc to the SW. This probably represents enhanced mass loss, also seen in the IR by Kervella et al. (2009, 2011). The mass loss mechanism for a massive star like Betelgeuse just entering the red supergiant phase is rather mysterious, as there is not enough dust close to the star for radiation pressure on grains to drive a wind. The average brightness temperature of the radio photosphere at 5-6 GHz is about 1200 K, but e-MERLIN resolved two hotspots at 4000-5000 K. This is higher than the peak temperature of the optical photosphere (3600 K). The hot spots could be due to Betelgeuse's patchy chromosphere which is known to have a low filling factor (Harper et al. 2006), or to convection or pulsation shocks. Further work will identify which mechanism is responsible and the relationship with processes which could eject clumps of matter from the stellar surface to form the wind.
These results will be presented in a forthcoming publication and at the Betelgeuse Workshop 2012
The observations were made by A. M. S. Richards, R.J. Davis, S.T. Garrington, I. McDonald (University of Manchester), S. Etoka (University of Manchester and Hamburger Sternwarte), L. Decin (Katholieke Universiteit Leuven), J. J. Lim (University of Hong Kong and Academia Sinica) and Markus Wittkowski (ESO).
e-MERLIN's deep radio survey of the Hubble Deep Field: First results
27 Mar 2012
27th March 2012: e-MERLIN's deep radio survey of the Hubble Deep Field: First results
A team of astronomers at Jodrell Bank Observatory have begun the deepest ever high-resolution radio imaging of the region around the Hubble Deep Field (HDF), the images originally captured by the Hubble Space Telescope (HST) in the mid 1990s. The HDF led to the discovery of numerous galaxies billions of light years distant and provided direct visual evidence of the evolution of the Universe. First results from the new imaging, which uses observations from the UK's newly upgraded e-MERLIN radio telescope array together with the EVLA radio array based in New Mexico, show galaxies some 7 billion light years away in unprecedented detail. Graduate student Nick Wrigley will present the new results at the National Astronomy Meeting in Manchester on 27 March 2012.To read the full press release.
e-MERLIN Cycle-0 online simulator tool
12 Jan 2012
12th January 2012: e-MERLIN call for proposals Cycle-0 (semester 2012A)
A new web-based simulator designed to assist in proposal preparation for e-MERLIN, cycle-0 and beyond is now available at http://www.e-merlin.ac.uk/observe/eMERLINost.html
This easy to use simulator tool allows sensitivities, uv-coverages and simulated images to be produced to aid with all forms of e-MERLIN proposals.
e-MERLIN Cycle-0 (semester 12A) proposal submission tool is open
10 Jan 2012
10th January 2012: e-MERLIN call for proposals Cycle-0 (semester 2012A)
e-MERLIN is now open to proposals from the international astronomical community on the basis of scientific merit alone. Proposals are competitively peer-reviewed under standard STFC rules by the PATT e-MERLIN Time allocation Committee
The e-MERLIN proposal submission tool Northstar is now open for proposal submissions for Cycle-0
Proposal deadline = Midnight (23:59GMT) 26th January 2012
5 Jan 2012
5th January 2012: A boost for European Radio Astronomy
A boost for European Radio AstronomyThe European astronomy collaboration RadioNet has been granted 9.5 million Euros by the European Commission to fund its latest program, RadioNet3, for the years 2012 to 2015. This not only continues the two preceding European projects, but also takes a leap forward to include ALMA, as well as a number of pathfinder pro grams for the SKA. Read the full press release at the MPIfR site.
10 Jan 2012
10th January 2012: e-MERLIN call for proposals Cycle-0 (semester 2012A)
e-MERLIN announces first open call for proposals
12 Dec 2011
12th December 2011: e-MERLIN call for proposals Cycle-0 (semester 2012A)
e-MERLIN is now open to proposals from the international astronomical community on the basis of scientific merit alone. Proposals are competitively peer-reviewed under standard STFC rules by the PATT e-MERLIN Time allocation Committee. During the first 5 semesters of e-MERLIN operations ~50% of observing time has been allocated to 12 large legacy projects and most of the remaining time will be allocated via PATT to standard proposals solicited prior to each observing semester. e-MERLIN provides high resolution (40-150mas) and high sensitivity (~6-12 uJy in this cycle 0) imaging at cm wavelengths as well as polarimetry, spectroscopy and astrometry. Shared-risk 'Cycle-0' observations will start in February 2012, with some limitations in observing capabilities.
Black holes and warped space: New UK telescope shows off first images
9 Dec 2010
9th December 2010: Black holes and warped space: New UK telescope shows off first images
This dramatic image is the first to be produced by e-MERLIN, a powerful new array of radio telescopes linked across the UK.
Spearheaded by the University of Manchester's Jodrell Bank Observatory and funded by the Science and Technology Facilities Council, the e-MERLIN telescope will allow astronomers to address key questions relating to the origin and evolution of galaxies, stars and planets.
To demonstrate its capabilities, University of Manchester astronomers turned the new telescope array toward the "Double Quasar". This enigmatic object, first discovered by Jodrell Bank, is a famous example of Einstein's theory of gravity in action.
The new image shows how the light from a quasar billions of light years away is bent around a foreground galaxy by the curvature of space. This light has been travelling for 9 billion years before it reached the Earth. The quasar is a galaxy powered by a super-massive black hole, leading to the ejection of jets of matter moving at almost the speed of light - one of which can be seen arcing to the left in this new e-MERLIN image.
The e-MERLIN image is shown in false-colour with a colour table ranging from blue through red to white, where the colours represent the bri ghtness of the radio emission. The HST image is made from WFPC2 images through two filters: the F555W filter (V-band) is coloured green and the F 814W filter (I-band) is coloured red.
Credit: Jodrell Bank Centre for Astrophysics, University of Manchester