Wednesday, 19 December 2018

Jupiter's Equatorial Disturbance Cycle

Tuesday, 18 December 2018

H2S on Neptune?

Wednesday, 5 December 2018

Research Associate in Planetary Atmospheric Science 2019

Department of Physics and Astronomy, University of Leicester
Full Details: 
Salary Grade 7 - £34,189 to £39,609 per annum
Funding is available from 1 March 2019 to 31 March 2022
Closing date:  14 January 2019

The Physics and Astronomy Department at the University of Leicester invites applications for a Post-Doctoral Research Associate (PDRA) in Planetary Atmospheric Science.

You will join the planetary atmospheres team led by Dr Leigh Fletcher to address the scientific aims of a European Research Council (ERC) grant to explore time-variable processes shaping the atmospheres of the giant planets.

The “GIANTCLIMES” programme seeks to investigate the natural cycles of meteorology, circulation, and chemical processes shaping the environments of the four giant planets over long spans of time. Inversions of planetary spectra, from the ultraviolet to the microwave, will be used to reconstruct these atmospheres in three dimensions to explore their temporal variability and the processes coupling different atmospheric regimes. Potential sub-projects include, but are not limited to: analysis of multi-instrument data from the Juno and Cassini spacecraft; assessments of the chemical distributions and radiative energy budgets of the four giants; numerical simulation of periodic and stochastic meteorological events (including wave phenomena); spectroscopic mapping techniques from Earth-based observatories; and assembly of data analysis pipelines to support “Guaranteed-Time” and “Early-Release” science activities ahead of the launch of the James Webb Space Telescope.

You will be expected to carry out independent and collaborative research for this project and disseminate the results to the international scientific community. There will be significant opportunities to collaborate within the Leicester’s Planetary Science team (whose existing research includes planetary magnetospheres, ionospheres, atmospheres and surface science), and with an international team specialising in radiative transfer and spectral inversion for planetary atmospheres.

In addition to the online application form, applicants are requested to provide: [1] a CV and publication list; [2] two academic references; [3] a one-page cover letter detailing how your prior experience and future research aims are commensurate with the aims of the programme outlined above.

Informal enquiries are welcome and should be made to Dr Leigh Fletcher on or 0116 252 3585

Thursday, 9 August 2018

Report on COSPAR Ice Giants Session

COSPAR Symposium B5.4 – Wednesday July 18th 2018
Ice Giant Systems:  New Results and Future Exploration
MSO: Leigh Fletcher (Univ. of Leicester)
DSO:   Amy Simon (Goddard Spaceflight Center)

COSPAR sub-commission B5 hosted several symposia focussing on the exploration of the outer solar system at the 2018 COSPAR meeting in Pasadena, ranging from the highlights of past missions (Cassini), active missions (Juno), and future missions (exploration of ocean worlds).  The ice giant community met on Wednesday afternoon to focus on the exploration of Uranus and Neptune, from their interiors, to their atmospheres, magnetospheres, rings and satellite systems.  Unusual for the COSPAR symposia, the organisers split the time between standard oral presentations and a workshop-style discussion forum on international collaboration for a future ice giant mission.  Both sections were well received and fostered interesting discussions between conference delegates for the remainder of the COSPAR meeting.

New Scientific Results

The ice giants, Uranus and Neptune, have been visited only once by a robotic spacecraft (Voyager 2 in 1986 and 1989, respectively).  Many of the most recent insights into how these unusual systems work are therefore the result of Earth-based observations, both from ground-based observatories and space telescopes. Hoftstadter et al. contrasted radio-wave observations of Saturn and Uranus from facilities like the Very Large Array (VLA), explaining how spectral models are used to explore the deep abundances of ammonia, hydrogen sulphide and (potentially) water within these worlds.  The existing Uranus data sensing the atmospheric composition can be explained by approximately solar abundances of these heavy materials, raising the question of how the materials might be trapped within their deeper interiors.  Wong et al. described Hubble Space Telescope observations of a new dark oval that formed on Neptune in 2015, not dissimilar from the Great Dark Spot observed by Voyager in 1989.  This oval has been re-observed several times since 2015 as it drifted southwards, whereas most drift equatorward.  Its bright companion clouds have become more centred within the vortex, and Wong’s team plans to track its continued evolution in the coming years.

Observations at mid-infrared wavelengths, sensing the atmospheric temperatures and composition of Uranus and Neptune, featured significantly for the rest of the symposium, largely as a result of preparation for the expected slew of data from the James Webb Space Telescope, due for launch in 2021.  Orton et al. presented images of Uranus at wavelengths sensing stratospheric emission from acetylene gas.  This provides a capability inaccessible to Voyager – the ability to probe the circulation of Uranus’ stratosphere.  The results, from the Very Large Telescope (VLT) and Gemini Observatory, indicate an unusual circulation pattern that localises the stratospheric emission to Uranus’ poles at the time of the 2007 equinox.  Fletcher et al. followed this up in a subsequent talk using spatially-resolved mid-infrared spectroscopy of Uranus, which is extremely challenging from Earth but whets the appetite for future data from the MIRI 5-28 µm instrument on JWST, which will provide the first
spatially-resolved spectra at these wavelengths.  Fletcher also presented VLT observations of Neptune, characterising stratospheric temperatures within its warm polar vortex during Neptune’s southern summertime conditions.  Sinclair et al. presented further stratospheric imaging of Neptune from the VLT, correlating diffuse warm regions in the stratosphere with cloud activity observed in the troposphere.  Finally, a poster by Rowe-Gurney et al. explored longitudinal variability observed in Spitzer Space Telescope disc-averaged spectra of Uranus, but not Neptune, hinting at unexpected dynamic variability on a world usually thought of as stagnant and inactive.

The scientific presentations continued with Masters et al. explaining how the processes governing ice giant magnetospheres might be rather different from those at work on the gas giants, presenting models indicating the important role of a viscous-like interaction between the solar wind and the magnetosphere.  Kirchoff et al. contrasted impact cratering size distributions on the Uranian satellites with those on Jupiter and Saturn, advocating future exploration of these terrains.  And Mandt et al. concluded the scientific discussion by exploring how measurements of the deuterium and nitrogen content of Triton’s atmosphere could prove crucial in understanding the origin of volatiles on distant worlds, including Pluto.

Future Exploration

The final hour of the symposium shifted into a discussion of future international collaboration on missions to the ice giants, hosted by Hoftstadter, Simon and Fletcher.  Hofstadter reported the primary outcomes of the 2016-17 NASA-ESA Science Definition Team study, which concluded in 2017 with an extensive report (  Simon described a recent white paper advocating a two-mission concept, combining a Uranus flyby with a KBO mission, alongside a dedicated Neptune-Triton orbital mission (  It was stressed that this was one of many potential ice giant exploration strategies, and concepts for Uranus orbital exploration were also discussed.  There was discussion of the criticality of planetary entry probes (, combined with orbital remote sensing in the infrared and microwave, in order to explore the chemical composition of Uranus and Neptune for comparisons with other targets in the solar system. 

Several ideas were raised during the wide-ranging discussion, including the need to identify and develop key enabling technologies for future ice giant missions, and how to ensure that ice giant science remained at the top of the agenda in the US Decadal Survey, ESA’s Cosmic Vision, and within the sites of other space agencies.  Particular attention focussed on how to open up the US medium-class missions (New Frontiers) to allow for ice giant exploration and on starting a new large-class mission before the next Decadal review.  Given the breadth of ideas, and the timescale for the next US decadal and future potential ESA studies, it was suggested that a dedicated ice giant workshop be held in 2019, to be used as a focal point for the development of topical white papers.  The discussion section was warmly received, and we would encourage similar events be worked into the programme for future COSPAR symposia.


Monday, 25 June 2018

James Webb Space Telescope to Target Jupiter's Great Red Spot

NASA’s James Webb Space Telescope, the most ambitious and complex space observatory ever built, will use its unparalleled infrared capabilities to study Jupiter’s Great Red Spot, shedding new light on the enigmatic storm and building upon data returned from NASA’s Hubble Space Telescope and other observatories.  Eric Villard wrote this piece on our proposed JWST MIRI observations of Jupiter: 

Jupiter image taken by Hubble Space Telescope
This photo of Jupiter, taken by NASA’s Hubble Space Telescope, was snapped when the planet was comparatively close to Earth, at a distance of 415 million miles.  Credits: NASA, ESA, and A. Simon (NASA Goddard)

Jupiter’s iconic storm is on the Webb telescope’s list of targets chosen by guaranteed time observers, scientists who helped develop the incredibly complex telescope and  among the first to use it to observe the universe. One of the telescope’s science goals is to study planets, including the mysteries still held by the planets in our own solar system from Mars and beyond.

Leigh Fletcher, a senior research fellow in planetary science at the University of Leicester in the United Kingdom, is the lead scientist on the Webb telescope’s observations of Jupiter’s storm. His team is part of a larger effort to study several targets in our solar system with Webb, spearheaded by astronomer Heidi Hammel, the executive vice president of the Association of Universities for Research in Astronomy (AURA). NASA selected Hammel as an interdisciplinary scientist for Webb in 2002.

“Webb’s infrared sensitivity provides a wonderful complement to Hubble visible-wavelength studies of the Great Red Spot,” explained Hammel. “Hubble images have revealed striking changes in the size of the Great Red Spot over the mission’s multi-decade-long lifetime.”

Fletcher and his team plan to use Webb’s mid-infrared instrument (MIRI) to create multispectral maps of the Great Red Spot and analyze its thermal, chemical and cloud structures. The scientists will be able to observe infrared wavelengths that could shed light on what causes the spot’s iconic color, which is often attributed to the sun’s ultraviolet radiation interacting with nitrogen, sulfur and phosphorus-bearing chemicals that are lifted from Jupiter’s deeper atmosphere by powerful atmospheric currents within the storm.

Fletcher explained that using MIRI to observe in the 5 to 7 micrometer range could be particularly revealing for the Great Red Spot, as no other mission has been able to observe Jupiter in that part of the electromagnetic spectrum, and observations in such wavelengths are not possible from Earth. Those wavelengths of light could allow the scientists to see unique chemical byproducts of the storm, which would give insight into its composition.

“We’ll be looking for signatures of any chemical compounds that are unique to the [Great Red Spot]…which could be responsible for the red chromophores,” said Fletcher. Chromophores are the parts of molecules responsible for their color. Fletcher added, “If we don’t see any unexpected chemistry or aerosol signatures…then the mystery of that red color may remain unresolved.”

Webb’s observations may also help determine whether the Great Red Spot is generating heat and releasing it into Jupiter’s upper atmosphere, a phenomenon that could explain the high temperatures in that region. Recent NASA-funded research showed that colliding gravity waves and sound waves, produced by the storm, could generate the observed heat, and Fletcher said Webb might be able to gather data to support this.

Close-up of the red spot on Jupiter as seen by the Juno spacecraft,
This true-color image of Jupiter’s Great Red Spot was created by citizen scientist Björn Jónsson using data from the JunoCam imager on NASA’s Juno spacecraft.  Credits: NASA/JPL-Caltech/SwRI/MSSS/Björn Jónsson

“Any waves produced by the vigorous convective activity within the storm must pass through the stratosphere before they reach the ionosphere and thermosphere,” he explained. “So if they really do exist and are responsible for heating Jupiter’s upper layers, hopefully we’ll see evidence for their passage in our data.”
Generations of astronomers have studied the Great Red Spot; the storm has been monitored since 1830, but it has possibly existed for more than 350 years. The reason for the storm’s longevity largely remains a mystery, and Fletcher explained that the key to understanding the formation of storms on Jupiter is to witness their full life cycle — growing, shrinking, and eventually dying. We did not see the Great Red Spot form, and it may not die anytime soon (though it has been shrinking, as documented by images from NASA’s Hubble Space Telescope and other observatories), so scientists must rely on observing “smaller and fresher” storms on the planet to see how they begin and evolve, something that Webb may do in the future, said Fletcher.

“These particular observations will reveal the storm’s vertical structure, which will be an important constraint for numerical simulations of Jovian [Jupiter] meteorology,” he explained. “If those simulations can help explain what Webb observes in the infrared, then we’ll be a step closer to understanding how these gigantic maelstroms live for so long.”

The James Webb Space Telescope will be the world's premier space science observatory. Webb will solve mysteries of our solar system, look beyond to distant worlds around other stars, and probe the mysterious structures and origins of our universe and our place in it. Webb is an international project led by NASA with its partners, the European Space Agency (ESA) and the Canadian Space Agency (CSA).

Sunday, 27 May 2018

#VLTJupiter 6: A Tour of Cerro Paranal

The first glimpse of the VLT came as our bus arrived at the Residencia from Antofagasta.  Four gleaming silver boxes on top of a flattened mountain.  We couldn't wait to get up there to see inside, so took the "Star Trail" path up to the summit on our second day.  This dusty path took around an hour, looping around to the west of the mountain to give us good views of the Pacific Ocean, albeit obscured by clouds held near the ground by an inversion layer.  The first thing you come to is the control building, over three stories high but beneath the main level.  This is where the astronomers sit, night after night, with control panels for each of the Unit Telescopes (UTs).  Take a gantry staircase up to the top, and you arrive at one of the most sophisticated and awe-inspiring telescope sites in the world.

Credit:  Iztok Boncina/ESO

The Telescopes

A map of the Paranal site, from the Residencia up to the VLT platform.

The four UTs, Antu, Kueyen, Melipal, and Yepun, each stand over 28.5 m high, each containing the 22-tonne 8.2-m diameter primary mirrors - single, monolithic mirrors, as large as we can build them with our technology today, made from a special glass-ceramic with almost no thermal expansion, called Zerodur.  These are mountain on a 350-tonne alt-azimuth mount, with a 1.1-m diameter beryllium secondary mirror to reflect the light back to the instruments at the Cassegrain focus.   Active optics with 150 supports control the shape of the thin (177 mm thick) primary mirror.  We got to go inside UT3 just as the sun was setting, and seeing this huge structure moving and rotating with very little sound was quite incredible.  We stood in total darkness, until suddenly the huge dome doors opened up, letting the moonlight flood in.  The wind shields behind the dome doors then opened one by one, as well as the vents all around and below the telescope - this lets the air in to keep the optics down at the ambient temperature of the mountaintop.  The dome rotates silently to align with the chosen target, and the alt-azimuth mount slews to the right elevation.  This is astronomy on an industrial scale.

Watching these huge UTs move around was an absolute privilege, especially with the golden glow of sunset in the background, Venus setting, and Jupiter rising in the east.  By the time we'd finish each night, Saturn was also high up in the sky.

The four UTs aren't the only things up on the platform - there are four additional 1.8-m telescopes called the ATs (auxiliary telescopes).  These are dedicated to full time interferometry, being able to move the ATs around on rails to produce a variety of different baselines (the further apart they are, the finer the scales they probe).  The UTs can also be used for interferometry, increasing the light collecting power, but it means that they're all being used at the same time on the same object, and no one else can use the instruments.  The beams from each telescope are combined in "delay lines" beneath the platform, where they are fed into different instruments.

ESO/H.H. Heyer

Happy Birthday

While we've been here at Paranal, UT1 celebrated a very special anniversary - it achieved first light exactly 20 years ago, on May 25th 1998, and in excess of 330 million EUR were spent in ESO Member States for the construction of the VLT.  The other UTs followed:

UT2, Kueyen: 1 March 1999
UT3, Melipal: 26 Jan 2000
UT4, Yepun: 4 September 2000

The annual budget is 16.9 million EUR without personnel costs, You can see recent 360-degree images of the summit here, and take a virtual tour here.  This website showing the current conditions is extremely useful.

"There's no cause for alarm.... but there probably will be."

Saturday, 26 May 2018

#VLTJupiter 5: A Tour of the Southern Sky

One of the incredible things about being on top of Cerro Paranal is the stunning visibility of the night sky and the Milky Way.  And for someone born and raised in the northern hemisphere, things can look decidedly odd.  The first thing that you notice is the moon, with the typical distribution of Mare and craters appearing upside down as viewed from the southern hemisphere.  Orion, typically a winter constellation for us, is visible at sunset from Chile.  But it's tipped over on its side, like a drunken archer, falling into the Pacific Ocean, Betelgeuse first.

Credit: ESO/Y. Beletsky

Our supporting astronomer, Florian, took us outside to see the night sky, standing in the shadow of UT1.  He pointed out Alpha Centauri 4.37 light-years away, and made the excellent point that our Sun would look exactly the same if we were standing on a planet orbiting that star, towards the constellation Cassiopeia.  Just above this bright star is the Southern Cross, although I didn't spot it at first - I was expecting five stars in a cross shape, but it's actually four stars in a kite shape.  The long axis of the Southern Cross points then towards the southern celestial pole - no pole star there, like there is in the northern hemisphere.  Just below the Cross was a darker region of the Milky Way - this was the Coalsack Nebula, 600 light years away, and blocking out the light from the galaxy.

Bruno Gilli/ESO -

Looking to the southwest, we could see Sirius and Canopus (second brightest star in the sky after Sirius), and using 1.5x the distance between them, following the line south, I say a breathtaking sight - my first ever view of the Large Magellanic Cloud (a dwarf galaxy orbiting the Milky Way), as a fuzzy blob south of the main band of the Milky Way.  I never knew these could be seen with the naked eye, they're quite the sight!

A lot of the objects can be identified using the website.

#VLTJupiter 4: Observing with VLT

Observing from a large telescope is a rather different experience to what you might imagine.  It's not a case of being outside with the equipment, your eye to the eyepiece, capturing your data.  We're sat in a control room several floors below the VLT platform, with UT3 doing its work remotely on the mountain top.  In fact, all the telescopes are controlled from here - there are horseshoe-shaped desks for each telescope (the UTs), each one with a telescope operator, the support astronomers and, in our case, space for the visiting astronomers.  There's also space for the ELT (which will be controlled from here, even though its platform, Cerro Armazones, is kilometres away) and the interferometry.  It’s all very high-tech, but essentially a large open plan office where the astromers sit for the full night.

We have dinner in the Residencia at around 5pm, then drive the 10 minutes up the mountain in ESO's fleet of old, slow Fiat Puntos.  Sunset happens pretty fast at this latitude of 24S, so we head up to the VLT platform to watch the sun vanish over the Pacific ocean, shrouded in an array of brightly coloured clouds.  In fact, the clouds always obscure the ocean itself, hiding it beneath an unending mat of white.  To the east, deep purples and pinks show the shadow of the mountain, with Jupiter rising (we're really close to opposition right now).  Venus has been glowing bright as the Sun disappears, but there's little time to waste as we head back down to the control room.

VISIR Observation Strategy

Padraig and I have had a plan each night for the sequence of VISIR 5-20 µm observations, with the ultimate aim of using Jupiter's ten-hour rotation to map out as many longitudes as possible, generating full maps of the planet in lots of different spectral settings.  The benefit of mid-infrared observing is that we don’t need to wait until it gets dark to start taking data - the sky is always bright in the mid-IR.  We can start during twilight, which ends around an hour after sunset.  The telescope operator, Ben, would find a nearby bright star to guide on and to perform the "active correction" - deforming the main 8.2-m mirror with a series of actuators to correct for distortions caused by flexure and temperature changes.  Then our support astronomer, Florian, would load up the first of our observation blocks for execution.  These start with an acquisition template, a first glimpse of Jupiter so that we can move the telescope around a little, centring Jupiter, before starting the main observations.

Then it's a case of clicking go, and watching along as VISIR changes its filters and moves through the spectrum.  We have to get the timing right, as Jupiter's 10-hour rotation is surprisingly fast when you're running against the clock.  Sometimes we’ll break and do 20 minutes of "lucky imaging" (taking a video of the scene at 5 µm so I can then stack together only the sharpest frames, freezing the seeing), or 20 minutes of spectroscopy using VISIR's low-resolution mode.  These tend to need the most user intervention, but for the rest of the time it's a matter of making sure that nothing is going wrong as the images are acquired.

Staying Awake

There's been some moments of excitement.  On our first night, we were taking data at exactly the same time as Juno was executing its close flyby.  That meant that we caught the flyby longitude (29W) perfectly, about 45 minutes before Juno flew over it on the terminator.  We spotted that Juno flew over one of the 5-micron hotspots on the North Equatorial Belt, the first time that's been accomplished during the mission.  We also had several opportunities to view the Great Red Spot in all its glory - the GRS is really unusual at the moment, after the passage of the South Tropical Disturbance.  It looks like a spoon holding an egg.  And the southern aurora was really vivid in all of our images (not so the northern aurora).  These all brought gasps from the other astronomers in the room - I don't think any of them are used to being able to see such incredible data in the raw images.

Glenn and colleagues were also observing on Subaru for two of the nights, so at one point we had a live Skype conversation going as VISIR finished its Jupiter observations and COMICS picked them up from Hawaii - two of the world's best observatories working in tandem.  We also had the Oxford service mode run on MUSE operating one night, so both UT3 and UT4 were looking in the same direction.

But there were some bad moments too.  To get decent images of Jupiter we really want to be chopping the telescope by more than 45 arcseconds, but we've always been limited to 25 arcsec in the past.  We tried to be cheeky and push this to 30 for some observations, which worked on the first night, but on subsequent nights it caused severe upsets.  The M2 mirror lost all power and had to be rebooted - literally turning it off and on again to get it working, which meant we lost 30-60 minutes of time on the second night.  Furthermore, the spectroscopy and burst mode imaging with VISIR proved to be exceedingly difficult.  I spent most of my daytime hours trying to figure out the complexities of their reduction, coming back to the mountain the next night with suggestions for improvements.  On the plus side, we'd be experts in VISIR data acquisition by the end of the run….

The first couple of nights spoiled us with excellent conditions - low wind, perfect seeing, incredibly low water vapour.  Heading up on the mountain on the third night, we could see light cirrus overhead and the temperature had dropped.  We were going all-guns-blazing until around 21:30, when the wind went above 12 m/s, meaning that we had a 'pointing restriction' and had to turn the telescope away from Jupiter.  Above 18 m/s and they have to close, so we remained open, but executing service mode observations pointing away from the wind direction out of the north.  I can’t tell you how frustrating it is to sit watching the minutes (and Jupiter longitudes) flick by while we can’t observe…  but on the plus side, the support astronomers were generous.  When the wind dropped at about 1am, they gave us the extra few hours back, and we continued with Jupiter until around 4am in the morning.

Night's End

At the end of each half-night we'd hand back over to the interferometry mode, which uses all four Uts.  We'd collect our things and head outside to the Puntos, but it was astonishingly dark outside when the moon had set, providing us with a stunning view of the night sky, the Milky Way, and the Magellanic Clouds.  Almost enough to want to stay up longer, until sleep deprivation took its hold…

#VLTJupiter 3: ESO's Residencia

One of the most incredible things about this whole experience has been staying in the Residencia, about 300 m below the mountain peak in the middle of the desert.  This award-winning hotel has been in use since 2002, and will likely be expanded in the future to accommodate all the new users of ELT.  In fact, it was designed to be part of the landscape rather than to obscure it, being built below ground with only the south-facing windows and doors being visible.  From the outside, it's a long red-brown structure that blends in with the surrounding red-brown hills, with a white dome over the roof.  When the bus first pulls up, you end up going down a long ramp to a pair of thick, grey doors.  As soon as you open them, though, the arid desert vanished and you enter the tropics, at the top of a long spiralling ramp that takes you down to the reception desk.

The south facing rooms of the Residencia.

In the centre of this curved walkway is a tropical oasis, with palm trees, colourful flowers, and even birds flying from plant to plant.  Right in the middle is a swimming pool, which I haven't seen used at all during my stay, but which I'm told is there to help the humidity of the building.  Nearby are comfy chairs, a table-tennis table, and table football.  For the musically inclined, there's a fully stocked music room next to a cinema/library room.   A row of offices for visiting astronomers looks out over the pool (I spent several hours sat in those offices getting work done during the day).

The rooms themselves are along a long, elongated stretch of building, with ramps rather than stairs running between floors.  My room faced south, with a door that you could open onto the silence of the desert.  In fact, apart from the footsteps of the odd passing astronomer, it was so silent in the Residencia - bliss when trying to work or get some sleep.  Food is served almost constantly in the canteen, which you scan in and out of - you could get very fat here, with so much on offer.  They even ship food up to the control room at night, so we dined on pizza and cake in the small hours of the morning, washed down with coffee to keep us awake.

The pool and reception area.  Credit:  P. Horálek/ESO

My interest in this building goes beyond just the gorgeous architecture.  I'm a huge James Bond fan, so it's wonderful to be staying in the "Perla de las Dunes", a "Bolivian" hotel and lair of the bad guy in Quantum of Solace.  That version was blown up by Bond in his climatic battle (in Pinewood, at least), but the exterior shots were all filmed here.  Lovely connection between my two loves - Bond and planetary science!  And being visitor number "007" was also quite a perk.

But back to astronomy  - on our first couple of evenings here, it was hard not to spend time outside gazing up at the night sky.  We'd go and sit in the shadow of UT5, the small public telescope near the hotel, blocking out the moonlight.  Again, the silence was perfect, and the stars spectacular.

Wednesday, 23 May 2018

#VLTJupiter 2: Journey to Paranal

Chaotic.  That's probably the best way to describe my second-ever trip to South America.  We were late boarding the flight from Heathrow having gotten confused between A and C terminals and having to run through the tunnels beneath the runway.  We were almost late boarding the flight from Madrid because the "transfer" signs weren't obvious and we ended going through the immigration counters twice.  And arrival in Santiago, at around 7.30am, was a nonsense - no idea where to collect baggage, enormous immigration queues, and even larger customs queues.  It took us a good couple of hours to escape the airport, find the TransVIP desk and get our cab out to the ESO Guest House in Las Condas, on the east side of Santiago.

Some of this was ameliorated by a very comfortable, modern airliner with LATAM - no window shades, but buttons used to change the opacity of the windows themselves!  And the view over the Andes at sunrise, as we came into land, was nothing short of spectacular:

I'm travelling with my 2nd-year PhD student, Padraig Donnelly, whose job it'll be to analyse the Jupiter data we acquire from the VLT.  We'll get to that, but for now, we had a whole Sunday to explore the beautiful city of Santiago.  The taxi to the guesthouse cruised along modern, broad freeways into a residential district west of Santiago, and we were immediately struck by the autumnal look of the place - orange and red leaves on the trees, quite the contrast to the springtime Britain that we'd left behind.  The guesthouse was a very laid-back affair:  three low-level wings of bedrooms, surrounding a central courtyard and fountain, with an unused swimming pool out the back.  There was a lounge with coffee machines, books, and a stereo, and a dining room where breakfast, lunch and dinner were served by the very friendly staff.

Exploring Santiago

After breakfast and a shower, we walked 15 minutes to the Escuela Militar underground station, purchasing a "BIP" card with enough credit for a return trip (about $3000 pesos) and travelling to Santa Lucia station.  From there we took a walking tour of the Centro district, half-remembered from the last time I visited Santiago in 2015.   We climbed the Santa Lucia hill, a landscaped region of gardens and statues, to reach the red-brick Torre Mirador at the summit, with its excellent panoramic views of the city and the Andes in the distance.  We found our way to the Mercado Central fish market, dined in the central "Agusto" restaurant on Sea Bass and prawns, fresh from the market stalls, and then wandered the shopping streets of the Centro district to do some people-watching near the Plaza de Armas and Catedral Metropolitana, right in the heart of the city.   Other than tourists, it was notable how peaceful the city was - almost all of the shops and businesses were closed, and it was great to see a country respecting Sunday as a day off work!

We returned to the Guesthouse via a bar near Escuela Militar, then wandered back in time for Pisco Sours at 18:45 (a time so regular that it was advertised on the wall of the guesthouse, next to the meal times).  We had a delicious 3-course meal in the dining room, meeting three other astronomers - two that had just returned from La Silla, and one who was about to travel to that observatory for the first time, and was excited as Padraig and I.

To Antofagasta!

Monday morning started at 5am, with a quick breakfast and shower, a taxi back to the airport, and an 8am flight north to Antofagasta.  This city, right on the Pacific coast and next to the Tropic of Capricorn at 23S, was previously part of Bolivia until the War of the Pacific in 1879-83, after which it was transferred to Chile.  In fact, we later discovered that today (May 21st) was "Navy Day", a national holiday in Chile, which explained why the city was quiet.  The landscape was dry and arid, as befitting a city in the Atacama desert, the driest place on Earth. An air-conditioned ESO coach picked us up at the airport and drove us into the city along the sea front, past the infrastructure of the port and the copper mining on which the economy was founded.   There we collected a few more people, and headed south into the desert and the mountains, along a smooth paved road through a desolate and dry landscape.  It was hard to escape the feeling that breaking down out here would be a VERY bad idea.

The coach continued south for a couple of hours, with very limited signs of any civilisation along the way.  Mountains were on either side of us, but the road followed a broad valley between them, before we branched off to the west and back towards the ocean.  The road climbed higher, along various switchbacks, until we finally caught a glimpse of what we'd been waiting for - in the distance, the gleam of four silver monsters sat upon the top of Cerro Paranal, the 2635-m high home to ESO's Very Large Telescope.  We stopped at the security lodge to collect our Visiting Astronomers badges, before descending into a tunnel under the desert soil - the entrance to ESO's astonishing Residencia building. 

Tuesday, 22 May 2018

#VLTJupiter 1: Jupiter from the VLT

Over the past decade, I've been exceedingly fortunate to have won time on the European Southern Observatory's (ESO) Very Large Telescope (VLT) to observe all four of the giant planets in the mid-infrared.  These observations, sampling thermal emission from 5 microns in the M band, to 10 microns in the N band, and 20 microns in the Q band, can reveal the three-dimensional temperatures, winds, gaseous composition and cloud structure, from the churning, convective tropospheres all the way into their stable stratospheres.  Many of my papers and projects have relied on this exquisite VLT dataset.

But despite all of that, I've never been able to visit VLT in person.  It's been an item on my bucket list for over ten years.  My observations were always in 'service mode', meaning that I'd design them in a piece of software (i.e., which filters to use, where to point, and for how long), then upload them to the ESO office to be put into a queue.  Those queued observations are then executed by supporting astronomers on the mountaintop, in between time-critical 'visitor mode' runs.  The trouble with this approach is that it's been hard to control the exact timing of the observations, and the data were usually taken within 1-4 weeks of when I actually wanted them.  For most datasets, that's been absolutely fine.  But now that the Juno spacecraft is in orbit around Jupiter, completing close flybys of the gas giant once every 53 days, the precise timing of my observations has become more critical.  So today (May 22), I'm writing this blog post from 2300m up on Cerro Paranal in the astronomer's residence, waiting to begin a visitor-mode run tomorrow night.

A map of the ESO sites in Chile - we flew from Santiago to Antofagasta, before a bus journey south along the B-710 to Cerro Paranal.  Cerro Armazones, the future home of the ELT, can be seen as a flattened mountain in the distance to our east.

The Juno Connection

The Leicester team are a part of an international network of planetary astronomers supporting NASA's Juno spacecraft in its exploration of Jupiter.  Juno has now completed twelve close passes around Jupiter known as perijoves, coming in over the north pole, sweeping within a few thousand kilometres of the equator, then exiting high over the south pole.   The thirteenth such encounter is on May 24th at 05:40UT, approximately 48 hours from now.  Now, Juno has been doing some tremendous science, but its science questions are focussed, and there are gaps in capability within the payload.  The Earth-based programme has been providing support in three broad areas:

  1. Spatial context:  Juno has a close-in view of dynamic phenomena and weather systems as it flys north-south across Jupiter, and can't always see the wider context of the zone or belt in which that weather system is embedded.  In contrast, our data can view the whole planet at once, providing the global perspective.
  2. Temporal context:  Jupiter's weather and auroral processes can evolve significantly between the perijoves, with new storms erupting, vortices interacting, belts fading and expanding, and aurora shifting and changing in response to a variety of processes in the magnetosphere and solar wind.  The Earth-based programme catalogs these changes over short timescales (between perijoves) and long timescales (multiple years) to better interpret Juno's observations.
  3. Spectral context:  Juno does a fabulous job in the ultraviolet, visible (with imaging), 2-5 µm region (with imaging and spectroscopy) and 1.3-50 cm microwave region.  But there's nothing in the X-ray, 0.9-2 µm infrared, 5-25 µm thermal infrared, and the sub-centimetre range below 1.3 cm.  An army of Earth-based facilities, including Chandra, Hubble, VLT, Subaru, IRTF, VLA and ALMA, have been used over the past two years to plug this gap.  That's not to mention the amateur astronomers observing on a nightly basis.

Back in 2015, several representatives of these telescopes travelled to the ESO headquarters in Vitacura, near Santiago, for a week-long workshop on collaborations between ground-based astronomers and space missions.  I wrote about that meeting here.  As a result of this workshop, I led a white paper, addressed to the ESO Director of Science, that emphasised the timely nature of VLT and ALMA observations during the Juno mission, making the three points outlined above.  I like to think that they helped to smooth the way for the ESO proposals that ensued over the following three years, during which time we've been successful in winning service mode runs for Jupiter every semester.  These data will be useful for the Juno mission, but also for my work studying the long-term evolution of Jupiter's meteorology and climate.

And that brings me full circle to this silent mountaintop in northern Chile.  While we're working up here, I'm going to try to keep a record (who know's whether I'll ever have the chance to return!), to give a flavour of what it's like.  And that starts with the journey.

Current location - 12 km from the sea, 2.3 km in the air, on top of Cerro Paranal.  Cerro Armazones is off to our east.

Tuesday, 13 March 2018

Discovery of Uranus and its Satellites

Wednesday, 17 January 2018

Midlands Alliances

Spurred by an "over-coffee" conversation about links between Midlands Universities, I discovered that a research and innovation partnership called "Midlands Innovation" brings together eight Midlands universities:

Their mission statement is to "drive cutting-edge research, innovation and skills development that will grow the high-tech, high skilled economy of the Midlands" by building "global hubs of research and innovation excellence", "exploiting the unique strengths and building on the rich history of collaboration of eight leading Universities across the Midlands: Aston, Birmingham, Cranfield, Keele, Leicester, Loughborough, Nottingham and Warwick." 

They point out that the "Midlands is at the heart of the UK, with a population of more than 11 million, creating £222 billion Gross Value Added – more than 14% of the total for the UK. It is also a high-export economy, with exports worth more than any other region in the UK – £49 billion annually, 17% of the UK total.  The region is at the heart of UK manufacturing and advanced engineering, accounting for 20% of UK manufacturing output through world leading business and industry like Alstom, Bombardier, Jaguar Land Rover, JCB, National Grid, Rolls-Royce, Tarmac and Toyota UK."  Midlands Innovation is tapping into "the Midlands Engine for Growth, the Government's ais to raise the long-term growth rate of the region, create hundreds of thousands of new jobs and add £34 billion to its economy by 2030."

A component of this is the Midlands Physics Alliance:  "a coordinated research group and joint Graduate School with the critical mass to compete with the top US and EU Universities.  The Alliance was established in 2007, with £5 million from the Engineering and Physics Sciences Research Council to invest in new, pioneering groups on cold atom physics. At its core, the Alliance consists of the Universities of Birmingham, Nottingham and Warwick. The Universities of Leicester and Loughborough are also represented on the Graduate School Steering Committee."

I hadn't been aware of any of these Midlands groupings, but it makes a huge amount of sense in an era of dwindling resources and diminished UK influence in the global arena.  The Midlands has a really strong technology base and the immense advantage of lower cost-of-living than the South of England - I think it's time that people heard more about these alliances!

Undergraduate Physics Research Internships

One of my roles at the University of Leicester is to manage the SURE Programme (Summer Undergraduate Research Experience), which provides opportunities for paid summer jobs working with our researchers in the Department of Physics and Astronomy.  Typically, we're able to offer 5-6 positions each year to 3rd-year undergraduates from the UK.  However, I receive something like 100 applications, meaning that I have to turn some 95% of applicants away.  I've never found a decent list of internship opportunities (maybe to whittle down to the most persistent undergraduates!).  But I'll do my best to keep a list here - no promises to keep it up to date!


Overseas and Open to UK Undergraduates:
  • Space Telescope Science Institute (STScI): Space Astronomy Summer Program [I benefited from this as an undergraduate in 2003, working alongside Dr. Frank Summers on an outreach project.]

Jupiter Update: January 2018

New year, and new views of Jupiter are rolling in.

John Rogers of the British Astronomical Society is always a wonderful source of insight as Jupiter changes its stripes (see his accounts of changes through the first ten Juno perijoves through to December 2017:, and this apparition has been no different, as he continues to comment on the images from amateur observers.  At the same time, Marco Vedovato continues to update his database of Earth-based maps (, with maps from Nov 2017 to today.

So far this year, he's noted "how rapidly the [North Equatorial Belt] is evolving, at least in this sector; the great waves have developed into a series of barges, and the northern half is rapidly fading.  The dark brown NEB has receded so far southwards in this image that I begin to wonder whether it will become as narrow as in 2011-12, leading to another spectacular NEB Revival in 2019." The pattern of cyclones (dark) and anticyclones (white) on the northern edge of the NEB look absolutely spectacular - they're one of the end states of the NEB expansion and contraction phase that we saw throughout 2017.

The southern edge of the NTB (North Temperate Belt) continues to be a vivid red - maybe a photochemically-produced red haze as a result of the 2016 plume activity.

In the southern hemisphere, the rifting to the west of the Great Red Spot appears to be continuing.... this might be the "...resumption of normal convective ('rifting') activity there, in which case the [South Equatorial Belt] will probably not fade this year."  There's also a deep-red barge sat in the brown SEB that appears rather dramatic.

Meanwhile, Juno is on its way for the 11th perijove encounter on February 7th, and with luck, we'll have a whole variety of Earth-based observatories (VLT included) pointing towards the giant planet...

January 16th 2018 image from Anthony Wesley.

Wednesday, 3 January 2018

PhD Studentships for 2018

Tips for Student Reviews/Reports

[Health warning: personal preferences may differ between researchers!]

One of the key skills being developed in an undergraduate or graduate degree is the ability to summarise and communicate complex ideas in a succinct and accessible way.  This is tested several times during the Physics degree course here at Leicester, and common mistakes can lead to lost marks.  Here's a list of my own personal preferences for reviews and reports, in case they're of use to the wider community.

  • Three Ts:  Tell them what you’re going to tell them; tell them; then tell them what you’ve told them.  Repetition of key points helps to reinforce them.  You’re telling a story.
  • Central Theme:  Use the introduction to define a central question or thesis that your review will address, and keep referring back to this in each Section and in the Conclusion.  That way, the reader will understand how each particular section fits into the wider review.
  • Summarise sections:  At the end of a section, before moving on, try to include a few sentences/statements to say where we are in the review – what is the take-home message of the previous section, and what are we going to look at next?  This helps to avoid abrupt transitions between sections.
  • Numbered Sections:  Use numbered sections and subsections to break up large sections of text, and to make it easy to refer both forwards and backwards to different sections (signposting).
  • Figures:  Make sure that figures are referred to in the main text, so that the reader knows when they should be looking at a particular chart, table, or diagram.  Ensure that the caption contains sufficient information to explain what the reader is seeing, and contains either a source (Author et al, yyyy) or a web URL for the origin.  Ensure figures have a sufficient size to be useful.
  • References:  Avoid references to ‘NASA’, ‘ESA’, ‘Met Office’, etc. – if the information came from a weblink without a distinct author/year, use a footnote to provide the link.  If the information came from a primary source, use the ‘Author et al., (yyyy)’ format and include in your bibliography.
  • Text boxes:  Sometimes definitions or brief digressions are required in a review, so make use of text boxes (placed in the document like figures and referred to in the main text) rather than breaking up the flow of the report.
  • Columns:  The use of two columns helps to break up large blocks of text and is easier on the eye.
  • Keep to the point:  Don’t be tempted to go off topic or to introduce information that isn’t relevant to the central theme of the project – this can just lead to confusion and dilutes your take-home messages.
  • Proof-read:  Read it over and over again, even out loud, to make sure that the sentences flow together and make the points you’re intending.