Live Chat with Chris Lintott and Rob Simpson about Galaxy Zoo Science

Yesterday I was involved in a live chat with Chris Lintott and Rob Simpson from The Zooniverse. We used a Google+ hangout to video chat about recent Galaxy Zoo science (my paper) and also answer questions from members of the public on future plans for Galaxy Zoo.

You can view the whole chat (30 minutes) on The Zooniverse YouTube Channel.

 

The Zooniverse plans more of these events, so let us/them know what you liked about it and what didn't work.

My latest paper accepted in MNRAS.

A cross posting from the Galaxy Zoo blog. I'm delighted to announce that the latest paper based on Galaxy Zoo classifications was accepted to appear in the Monthly Notices of the Royal Astronomical Society earlier this week, and appears on the arxiv this morning (link). Usually there is a long delay between submission and acceptance of papers (something Kevin discussed on the Galaxy Zoo blog in "What Happens Next - Peer Review"), but in this case the initial referee report came back after 2 days, and the paper was accepted only 2 weeks after the first submission so I never got time to post to the arxiv or write a blog post about it before it was accepted! This was certainly the smoothest and fastest referee process I've been through. ;) Here's the title page.

 

 So what was new about this paper was that we combined information on the morphologies (whether or not the spiral galaxies had bars) with information on the amount of atomic hydrogen gas the galaxies contained and and our main result was that galaxies with more atomic gas in them, are less likely to have a bar. But I want to back up a bit first and tell you about where we get this information on the atomic gas content, and why it  might be interesting. As you might guess from the title of the paper it's from something called the ALFALFA survey (and the new names in the author list for a Galaxy Zoo paper - Martha Haynes and Riccardo Giovanelli - are from Cornell University who are running this survey). Atomic hydrogen emits radio waves at a frequency of 1.4 GHz (or 21cm). This is detectable by a classic radio telescope (in what we call the "L"-band which makes up the second L of ALFALFA). In the case of ALFALFA, we use the Arecibo radio telescope (two of the "A"s in the acronym stand for Arecibo, the third is for array), which is the worlds biggest single dish radio telescope deep in the jungle of Puerto Rico.

Aerial shot of Arecibo. Credit: NAIC.

 ALFALFA is a massive survey which will map the location of atomic hydrogen over basically the whole sky visible to the Arecibo radio telescope. What's neat about a survey for something which emits as a specific frequency is that you actually get a 3D map of where the hydrogen is - both redshift and sky position! Anyway, we made use of about 40% of the survey which is already complete, and which covers about 25% of the area of the sky in which the Galaxy Zoo galaxies are found (the Sloan Digital Sky Survey Legacy Area). Adding some cuts on how face-on the galaxies are so that the bars can be identified, and to make sure the sample contains the same size galaxies right through it's volume we ended up with 2090 galaxies with both atomic hydrogen detections and bar classifications from you guys. This is an order of magnitude larger than any similar sample! So thanks. :) Atomic hydrogen is the basic building block of galaxies (after dark matter). It represents the fuel for future star formation in a galaxy - a galaxy with a lot of atomic hydrogen could in principle make a lot of new stars. Many spiral galaxies have a lot of atomic hydrogen (with perhaps as much as 10 times as much mass in hydrogen as in stars!), while a typical elliptical galaxy has very little atomic gas, and so cannot form lots of new stars. So our observation that bars are more likely to be found in spiral galaxies with less atomic gas supports our earlier ideas about bars possibly "killing" spirals (ie. helping to stop them form stars). 

Trends of bar fraction with atomic gas content, galaxy colour and how many stars are in a galaxy.

 Of course it's never quite that straightforward with galaxies. To start with correlation is not the same as causation, and to that we add that lots of things are correlated. We show some of that in the figure above. Bars are more likely in redder spirals which have more stars ("log Mstar" represents stellar mass in units relative to the mass of our Sun) and which also have less atomic gas. So the skeptical astronomer could say this has nothing to do with the gas content at all, just that the types/sizes of galaxies with less bars have more gas. To test that idea we measured the typical gas content of a spiral galaxy with a given number of stars, and from that we calculated how "deficient" or rich in atomic hydrogen any given galaxy was. Then we plotted the bar fraction against that. The convention in astronomy is to call how much less atomic hydrogen a galaxy has than normal it's "HI deficiency" which gets bigger the less atomic hydrogen there is (from the people who brought you the magnitude scale!).

Bar fraction against how much more or less atomic gas a galaxy has than is typical for the number of stars it has. Bigger HI deficiency = less atomic gas than is normal for a galaxy's size.

Example images.

 Anyway you can see we still see a clear trend, which demonstrates that it's likely to be the atomic gas driving the correlation. Where a galaxy is richer in atomic hydrogen than normal it's less likely to host a bar, and vice versa. Very atomic hydrogen rich galaxies which are massive and have bars are really quite rare! Here are some examples of low and high mass galaxies which are gas rich or poor and with or without bars. :) [/caption] I made images of the whole sample we use available here.

 At the end of the paper we put forward three possible explanations for the correlation, all of which fit in with the observations we presented. It's possible that the bars are causing the atomic gas in galaxies to be used up faster - "killing" the galaxy. The bar does this by driving the gas to the centre of the galaxy where it gets denser, turns into molecular hydrogen and from that stars (but only in the centre). It's also possible (based on dynamical studies of galaxies) that gas slows down the formation of a bar in a spiral galaxy, and/or destroys the bar. Finally it's possible that as a galaxy interacts with its neighbours, a bar gets triggered and its gas gets stripped (ie. the correlation between the two is caused by an external process). We'll need to do more work to figure out which of these (or which combination of them) is the most important.

 To my mind the most interesting result was a hint that if a gas rich galaxy does (rarely) host a bar, it's optically redder than similar galaxies without bars. It's just possible that bars hold back infall of gas from the outer regions of a spiral galaxy and slow down star formation over all in that galaxy. That idea needs testing, but if it's true it's saying that an internal structure like a bar plays an important role in the global star formation history of a galaxy.

 Anyway thanks again for the classifications! ;)

My favourite colour magnitude diagram

Cross post from the Galaxy Zoo blog.


I was embarrassed to discover today that I never got around to writing a full blog post explaining our work studying the properties of the red spirals, as I promised way back in October 2009. Chris wrote a lovely post about it "Red Spirals at Night, Astronomers Delight", and in my defense new science results from Zoo2, and a few other small (tiny people) things distracted me.

 I won't go back to explaining the whole thing again now, but one thing missing on the blog is the colour magnitude diagram which demonstrates how we shifted through thousands of galaxies (with your help) to find just 294 truly red, disc dominated and face-on spirals.

 A colour magnitude diagram is one of the favourite plots of extragalactic astronomers these days. That's because galaxies fall into two distinct regions on it which are linked to their evolution. You can see that in the grey scale contours below which is illustrating the location of all of the galaxies we started with from Galaxy Zoo. The plot shows astronomical colour up the y-axis (in this case (g-r) colour), with what astronomers call red being up and blue dow. Along the x-axis is absolute magnitude - or astronomers version of how luminous (how many stars effectively) the galaxy is. Bigger and brighter is to the right. So you see the greyscale indicating a "red sequence" at the top, and a "blue cloud" at the bottom. In both cases brighter galaxies are redder.

 The standard picture before Galaxy Zoo (ie. with small numbers of galaxies with morphological types) was that red sequence galaxies are ellipticals (or at least early-types) and you find spirals in the blue cloud. The coloured dots on this picture show the face-on spirals in the red sequence (above the line which we decided was a lower limit to be considered definitely on the red sequence). The different colours indicate how but the bulge is in the spiral galaxy - in the end we only included in the study the green and blue points which had small bulges, since we know the bulges of spiral galaxies are red. These 294 galaxies represented just 6% of spiral galaxies of their kind.

 So this is one of my favourite versions of the colour magnitude diagram.

What Types of Galaxies are in BOSS?

Over on the SDSS3 blog is a post about my recently accepted paper looking at the types of galaxies which are being observed in BOSS.

Copied below:

A critical question for the SDSS-III BOSS is what kinds of galaxies are they observing. In a recent paper by Masters et al., SDSS-III scientists used additional, higher resolution data from the Hubble Space Telescope (HST) to answer this questions.

In SDSS images, BOSS galaxies, which are on average about 6 billion light years away, just looks like fuzzy red blobs. The goal of BOSS is to observe 1.5 million of them over 30% of the sky in order to map the large scale structure in great detail. For this study, they took a look at a tiny subset of 230 of them which have deeper HST images (which were taken as part of the COSMOS project – the largest area HST survey every yet done).

The study found that 75% of BOSS galaxies are massive ellipticals, but that a surprisingly high fraction (20%) of these are split into multiple components in the HST images. The remaining 25% of BOSS galaxies are massive spirals.

The image below shows an example of one of the spirals and one of the ellipticals shown in both the SDSS and HST image.

As well as the paper, you can look at a poster about this work which was presented both at the AAS in Boston in May, and also at the recent Galaxy Formation conference in Durham

Finally if you want to browse all the images yourself they are available at www.icg.port.ac.uk/~mastersk/BOSSmorphologies/

Some recent Galaxy Zoo work

I'm a bit behind, but I wanted to point out two papers I was involved in from the Galaxy Zoo project which have recently come out on the arXiV.

Both were blogged about on the Galaxy Zoo blog (in both cases by the first author, and in both cases I was the second author).

Ben Hoyle: GZoo2 Bar Paper Accepted in MNRAS

Lucy Fortson: Galaxy Zoo and Zooinverse Review Article posted today on arXiv

This last ones use the above Hubble Tuning Fork I made using Galaxy Zoo style SDSS images of galaxies.