This is not a blog post as such, it’s the notes that I took during the conference split up into sections. Unfortunately there is no reference to the talk content itself; this is kept in the booklet which I have sitting next to me as I type this.

Session 1

Detecting and characterising via direct imaging

• More than 2Gyr gas giants more than 10^8 times fainter than primary
• Young stars are 10^4 - 10^7 times better than this
• Chronograph for increasing contrast
• Speckle noise a big problem
  • for speckle based data S/N does not increase with time
  • angular differential imaging
    • speckles oscillate while image rotates, but keep similar shape
    • real objects will move in the frame
• A stars good targets despite being bright
  • higher hosting fraction for giant planets for A stars (not sure about this)
  • high profile detections
  • Nielsen show low host fraction despite this
• M stars also good targets
  • despite low independent host fraction
• Typical contrasts - 10^5 at 1 arcsecond (with NICI)

Physical properties (atmospheres)

• Direct photons detected from these objects
  • reflected light and background contaminants surely?
• Colours in infra-red shows deviations from the predicted T dwarf type sequence (brightness vs colour)
  • more like L dwarfs
  • much lower surface gravity
• Direct spectra taken (!)
• Huge spectral diversity for planets even in same system
• Surface gravity strongly affecting the spectra
• Orbits of Beta Pic 2 - Chauvin et al. 2012
  • most probable semi major axis

Architecture

• Upper limits to abundance
• Cold start - less than 10% for separations 20 - 630 AU
• Hot start - less than 10% for separations 10 - 810 AU
• Gravitational instability planets rare at more than 10 AU
• Scattering planets also rare
• Sphere project - 10 - 80 more planets
• Possible detection of Super-Earth around nearby M dwarf (Crossfield, Goyon et al. 2013)

Summary

• Young exoplanets have red colours consistent with dusty clouds and non-equilibrium chemistry
• Hot start gas giant planets more than 4 MJup rare at more than 10AU

International deep planet survey

• Homogeneous analysis methods

SEEDS

• Strategic Explorations of Exoplanets and discs with Subaru
• Variety in morphology of protoplanetary discs
  • gaps, non-uniform shapes
• IRD - IR doppler instrument on Subaru
  • could be good for follow up for NGTS, investigate this
  • paper

Hershell dust evolution in discs

• SED modelling and Herschel tracing dust evolution in discs

###Planet formation in evolving protoplanetary discs

I’m currently on the plane back, flying over Canada at about 922km/h as the in-flight computer (android tablet in the back of the seat in front of me) says.

I’m sitting next to a nice chinese couple, who don’t speak a word of English. They asked me through vague hand gestures to fill out their immigration card. It was quite an ordeal!

Back home now after a good conference, got lots of nice pictures of Vancouver, but am quite tired now.

The last day has come and gone. I didn’t get time yesterday to write about it so I’m doing it now while I sit in front of the A-team in a Canadian hostel. As a side note this film looks terrible.

We had some of the most interesting talks of the day yesterday, talking about planet migration and feasibility studies. Some cool stuff but I still don’t have a disc migration based theory to explain the Rossiter-McLaughlin effect. A quite sensible talk was about the formation of hot Jupiters and how the primary migration mechanism is based on the host star (or disc) metalicity. Low metalicity stars can only cause hot Jupiters to migrate through type II migration due to lack of metals from which extra planets can be formed. High metalicity stars can support the same process, as well as dynamical formation as more planets will have formed from the protoplanetary disc. It kinda makes sense in my mind.

Today’s lectures were about… you guessed it: discs! A lot of people find them interesting apparently! Anyway the talks were ok, some good some bad. One in particular involved formation theories that seemed to explain the observed distributions well; I wanted to ask about selection effects but thought I’d find him afterwards. I didn’t have time in the end but it was very interesting.

Coffee was taken up by talking to a postdoc at UNSW about dynamical stability. We chatted for a while and it was nice. Lunch was an amazing experience: we heard about a great fish and chips place down by the harbour. It was not more than a shack and we were warned of the queues. We thought nothing of it and with a 2 hour lunch break had plenty of time. So we went down and queued for a while. A while being 1 hour 15 minutes. In the sun. I don’t get sunburnt very much but my face is quite red right now! By the time we’d finished eating it was time to return to the conference centre and resume the day. IT was fantastic food though, I’d recommend it if you’re visiting and have a couple of hours over lunch to space.

Today’s schedule was short, we had the afternoon off to do whatever we wished. Actually the conference organisers offered to put on a trip of some sort after a vote to find out the most popular choice, but that fell through as organising such a mammoth activity would be too difficult.

This session was the most relevant to me and my work, as it involved the observational side of things. We had some great talks from some friends of mine, and other colleagues in the field.

So today we learnt about discs, as the title of this post may suggest. We had protoplanetary discs (or proplyds which is a horrible portmanteau), thin discs, thick discs, transitional discs…

This mostly involved theorists and simulations working their hardest, but we did get a few observational results thrown in for good measure. To be fair it’s a simulation type topic, current methods are not powerful enough without some serious and therefore expensive time on the largest telescopes. Some nice analysis advances are being made but for once¹ observationalists have to play catch up.

So the first day has just finished. We had some interesting talks (and some not so interesting, but that’s to be expected).

The first session - before lunch - was dedicated to direct imaging, which is really taking off as a field, with advancements in technology and analysis tools since I last updated myself on the field. Being able to directly see protoplanetary disks is a new idea for me.

The ferry from Vancouver to Vancouver island (not Victoria island, as I’ve been told) was amazing. The scenery was breathtaking, photos of which I shall upload later. The little islands around Vancouver island were amazing to see, really fantastic. The map is centred on Victoria itself but the islands are to the north east.

We’re sitting on a coach waiting to depart to Victoria town centre, ready to find our hotel and work out where the conference centre is.

So we arrived at the hostel, a very nice place too. I’d recommend it if I could be bothered to find out what it is. I’ll try and remember to insert a reference here:

Reference

So yeah nice place. Vancouver is not very exciting so far but as was pointed out to me: the area around the airport is never going to be very nice.

The public transport on the other hand seems excellent so far. I’ll not get much of a chance to test it out, but from what I’ve seen so far it’s excellent. Fantastic public transport to and from the airport, something London sorely needs.

So we’re at the airport. Mostly uneventful journey so far, luckily. Airports terrify me; flying doesn’t scare me at all, but the chance of being rejected for something as simple as forgetting your passport is so unnerving.

I’ve been up since 6am this morning, which is pretty tough. I’ve managed to get some free wifi at the airport, ironically from BT Openzone which have announced that they’re closing to O2 customers. This is ironic for two reasons: