After two rounds of comments and questions from the journal referee, the first paper discussing the detailed results of the Hubble observations of the giant ionized clouds we’ve come to call Voorwerpjes has been accepted for publication in the Astronomical Journal. (In the meantime, and freely accessible, the final accepted version is available at http://arxiv.org/abs/1408.5159 ) We pretty much always complain about the refereeing process, but this time the referee did prod us into putting a couple of broad statements on much more quantitively supported bases. Trying to be complete on the properties of the host galaxies of these nuclei and on the origin of the ionized gas, the paper runs to about 35 pages, so I’ll just hit some main points here.
These are all in interacting galaxies, including merger remnants. This holds as well for possibly all the “parent” sample including AGN which are clearly powerful enough to light up the surrounding gas. Signs include tidal tails of star as well as gas, and dust lanes which are chaotic and twisted. These twists can be modeled one the assumption that they started in the orbital plane of a former (now assimilated) companion galaxy, which gives merger ages around 1.5 billion years for the two galaxies where there are large enough dust lanes to use this approach. In 6 of 8 galaxies we studied, the central bulge is dominant – one is an S0 with large bulge, and only one is a mostly normal barred spiral (with a tidal tail).<?p>
Incorporating spectroscopic information on both internal Doppler shifts and chemical makeup of the gas we can start to distinguish smaller areas affected by outflow from the active nuclei and the larger surrounding regions where the gas is in orderly orbits around the galaxies (as in tidal tails). We have especially powerful synergy by adding complete velocity maps made by Alexei Moiseev using the 6-meter Russian telescope (BTA). In undisturbed tidal tails, the abundances of heavy elements are typically half or less of what we see in the Sun, while in material transported outward from the nuclei, these fractions may be above what the solar reference level. There is a broad match between disturbed motions indicating outward flows and heavy-element fractions. (By “transported” above, I meant “blasted outwards at hundreds of kilometers per second”). Seeing only a minor role for these outflows puts our sample in contrast to the extended gas around some quasars with strong radio sources, which is dominated by gas blasted out at thousands of kilometers per second. We’re seeing either a different process or a different stage in its development (one which we pretty much didn’t know about before following up this set of Galaxy Zoo finds.) We looked for evidence of recent star formation in these galaxies, using both the emission-line data to look for H-alpha emission from such regions and seeking bright star clusters. Unlike Hanny’s Voorwerp, we see only the most marginal evidence that these galaxies in general trigger starbirth with their outflows. Sometimes the Universe plays tricks. One detail we learned from our new spectra and the mid-infared data from NASA’s WISE survey satellite is that giant Voorwerpje UGC 7342 has been photobombed. A galaxy that originally looked as if it night be an interacting companion is in fact a background starburst galaxy, whose infrared emission was blended with that from the AGN in longer-wavelength IR data. So that means the “real” second galaxy has already merged, and the AGN luminosity has dropped more than we first thought. (The background galaxy has in the meantime also been observed by SDSS, and can be found in DR12).
Now we’re on to polishing the next paper analyzing this rich data set, moving on to what some colleagues find more interesting – what the gas properties are telling us about the last 100,000 years of history of these nuclei, and how their radiation correlates (or indeed anti-correlates) with material being blasted outward into the galaxy from the nucleus. Once again, stay tuned!
While preparing for more observations of the Galaxy Zoo giant AGN clouds (Voorwerpjes), this is a good time to introduce more complete ways of obtaining astronomical spectra. Traditionally, we’ve put a long slit in front of spectrographs, so we can measure everything along that line without worries about overlapping spectra of different objects or pieces of sky. In some cases, as with the optical fibers used by the Sloan Digital Sky Survey, we get the light summed within a circular aperture on the sky (with Sloan, from hundreds of different objects at each pointing of the telescope). But many of the things we want to understand are large and oddly shaped, so these approaches limit us to a very partial view (or to making many observations to cover everything of interest). Enter the Integral-Field Unit (IFU), which is any kind of device that lets us get the spectrum of every point in some region of the sky. They often use fiber optics to rearrange light from the object, so each small region of it comes out at a different place on what would otherwise be the spectrograph slit. After that it all becomes a software problem.
IFUs are becoming more common on large telescopes. We’ve gotten excellent data on some Voorwerpje systems with the unit on the 8-meter Gemini North telescope. Here’s a sample of raw data on UGC 11185. Each horizontal streak is the spectrum of an area 0.2 arcseconds square. The sampling, sensitivity, and image quality are superb, revealing multiple clouds of gas moving within a total span of almost 1000 km/s.
On the other hand, if we want to use its whole wavelength range, the Gemini device covers only 3.5×5 arcseconds of sky at once. I’m headed to the 3.5m WIYN telescope on Kitt Peak to use a complementary device called Hexpak, newly commissioned by instrument designer Matt Bershady of the University of Wisconsin (who I’ve been emailing about this since I learned of the project three years ago). This fiber bundle plugs into the multipurpose spectrograph kept in a climate-controlled room below the telescope, and combines small and densely-packed fibers in the middle (for things like galactic nuclei, small and bright with lots of structure) and large fibers near the edges (collecting a lot of signal from large diffuse surrounding material – sound familiar?). Matt and his team were able to get a short exposure through thin clouds of UGC 11185 as a feasibility test – here’s a piece of that raw data frame, showing the small central fiber and the larger surrounding ones (which show brighter night-sky airglow lines as well as more object signal; the bright [O III] lines and H-beta are near the middle, with wavelength increasing to the right for each spectrum). I hope to get a lot more data like this shortly.
Elsewhere, the European Southern Observatory has commissioned an enormous IFU, and the Sloan team has rebuilt their fiber bundles so that each one now makes multiple IFUs which can be placed on many galaxies at a time – this part of the Sloan survey extension is known as MANGA. Then there is the Spanish-led CALIFA project for hundreds of galaxies, which has publicly released data for their first two subsets. Then there are SAURON (whose data ca be tamed in software by GANDALF) and the upgrade of SCORPIO-2 and more… Swimming in data as we sift for knowledge, I am reminded of this anonymous computer error message in haiku form:
Out of memory.
We wish to hold the whole sky
but we never will.
It was discussed within the science team once the nature of Hanny’s Voorwerp was becoming clear, since the color of that giant loop suggested similar emission-line properties at a larger redshift. Kevin gave it the name “Teacup” in honor of this loop. Then in March 2009, Georgia State University colleague Mike Crenshaw was here on my campus for a thesis defense. I showed him this object, and he mentioned that one of their graduate students was doing spectroscopy of active galaxies at the Lowell Observatory 1.8m telescope that week. Two nights later, Stephen Rafter from GSU obtained a long-slit spectrum crossing the loop and showed that it was, indeed, gas photoionized by an AGN. Later this object featured in the Voorwerpje hunt, as one of the 8 cases showing an energy deficit from the nucleus so it must have faded. Indeed, this example was a major factor in showing that the Hunt project would be worthwhile.
We’re in the middle of an observing run at the Lick 3m Shane telescope, with the first part devoted to polarization measurements of the Voorwerpje clouds (which is to say, giant clouds of ionized gas around active galactic nuclei found in the Galaxy Zoo serendipitous and targeted searches), and just now switching to measure spectra to examine a few new candidate Voorwerpjes, and further AGN/companion systems that may shed light on similar issues of how long AGN episodes last.
Polarization measurements can be pretty abstruse, but can also provide unique information. In particular, when light is scattered, its spectra lines are preserved with high fidelity, but light whose direction of polarization (direction of oscillation of its electric field when considered as a wave) is perpendicular to the angle it makes during this operation is more likely to reach us instead of being absorbed. This is why polarized sunglasses are so useful – glare from such scattering light can be reduced by appropriate orientation of the polarizing filter.
In our context, polarization measurements tell us something about how much of the light we see is secondhand emission from the AGN rather than produced on the spot in the clouds (admittedly as a side effect of the intense UV radiation from the nucleus), and will show us whether we’re fortunate enough that there might be a dust cloud reflecting so much light that we could look there to measure the spectrum of the nucleus when it was a full-fledged quasar. (This trick has worked for supernovae in our galaxy, which is how we know just what kind of supernova was seen in 1572 despite not having spectrographs yet).
Polarization wizard Sebastian Hoenig (now at the Dark Cosmology Center in Copenhagen) has already produced preliminary calibrations and maps from these new data. Here are some visualizations. In each case, the lines show the direction of polarization. Their length and color show the fraction of light which is polarized at points where there is enough to measure. This fractional polarization tells about the mix of light arising on the spot (even if secondhand due to UV radiation ionizing the gas) and that reflected from dust particles. There is a telltale annular or bull’s-eye pattern when the scattered light originates in a central source, which we see over and over (as if we hadn’t figured out to blame the galaxy nuclei anyway).
First up is a personal favorite, UGC 7342 (the last one to have its Hubble images obtained, and among the largest and brightest of the Galaxy Zoo sample).
The next one, Markarian 78, is less familiar, oddly because it makes perfect sense (so it has not figured much in the followup observations). In this case, we see a bright and obvious active nucleus, one which is powerful enough to light up the giant gas clouds without having changed over the past 60,000 years or so.
For comparison, here is a polarization map of IC 2497 and Hanny’s Voorwerp itself, from data obtained last year (the first time the weather let us get useful results). Sometimes we can hear the Universe laughing – a quick simulation shows that the reflected light from the nucleus, when it was a quasar, is just a bit too faint for us to have seen its signature broad emission lines in any of the Voorwerp spectra.
As we switch into measuring spectra for the next few nights, the aim changes to a combination of looking at a few new Voorwerpje candidates from the Galaxy Zoo forom, and a set of newly-identified AGN/galaxy pairs which may let us study the same issues of AGN lifetimes. We can sort of settle into a routine – Anna Pancoast does calibrations and setup during the day and hands over to Vardha Bennert to finish observations during the night. I typically get to work before Vardha finishes the last galaxy observation (thanks to the time-zone difference) and transfer data to start analysis, so we can change the next night’s priorities if something interesting shows up. It takes a (global) vllage, but then if there’s been any single meta-lesson from Galaxy Zoo, that would be it.
As usual when the American Astronomical Society meets, this has been an intense week of research results, comparing notes, and laying plans. Galaxy Zoo has once again been well represented. Here’s Kevin discussing the Green Valley in galaxy colors, making the case that it consists of two completely different populations when Galaxy Zoo morphologies are factored in:
Today we’re presenting first results of the Hubble imaging of Voorwerpje systems. This is what our poster looks like:
(or you can get the full-size 2.8 Mbyte PDF). We didn’t have room to lay out all the features we first had in mind, but these are the main points we make:
They show a wild variety of forms, often with filaments of gas stretching thousands of light-years. These include loops, helical patterns, and less describable forms.
The ionization, traced by the line ratio [O III]/Hα, often shows a two-sided pattern similar to the ionization cones around many AGN. This
fits with illumination by radiation escaping past a crudely torus-like structure. However, there is still less highly-ionized gas outside this whose energy source is not clear.
As in IC 2497, the parent galaxy of Hanny’s Voorwerp, many of these galaxies show loops of ionized gas up to 300 light-years across emerging from the nuclei, a pattern which may suggest that whatever makes the nucleus fade so much in radiation accompanies an increase in the kinetic energy driving outflows from its vicinity.
At the bottom of the poster we illustrate with new clarity a point we knew about in the original paper – for the two Voorwerpje systems with giant double radio sources, they completely break the usual pattern of alignment between the radio and emission-line axis. Mkn 1498 and NGC 5972 are aligned almost perpendicular, which can’t be fixed by changing our viewing angle. We’re speculating among ourselves as to how this could happen; maybe interaction of two massive black holes is twisting an accretion disk. But don’t quote me on that just yet.
The color images here show only the ionized gas, with [O III] in green and Hα in red. Starlight from the galaxies has been subtracted based on filters which don’t show the gas, so we can isolate the gas properties. The false-color insets show the [O III]/Hα ratio. The blank regions are areas whose signal is too low for a useful measurement. Red indicates the highest ionization, fading to deep blue for the lowest.
We were able to feature some new data that came in too late to be printed in the poster (by tacking up a smaller printed panel) – the long-awaited images of UGC 7342, among the largest and most complex clouds we’ve found (or more correctly, so many Galaxy Zoo participants found). Hubble observed it Monday afternoon, and after some frantic file-shuffling and processing, I got the data in the same shape as the others. And here it is:
Click on this one to see it larger. We barely know where to begin. The actual AGN may lie behind a dust lane, and there is a large region of very low-ionization as near it. Another loop near the nucleus, and fantastically twisted filaments winding their way 75,000 light-years each way.
There is still more to come – with Vardha Bennert and Drew Chojnowski, we planned the strategy for several upcoming observing runs at Lick Observatory (one starting only next week). These should include getting data on some of the most promising AGN/companion systems to look for the AGN ionizing gas in companion galaxies, and observation of regions in the Voorwerpjes that we only now see a context for. Additional X-ray and radio observations could fill in some of the blanks in our understanding. And by all means, stay tuned!
After a winding path, the first overlap paper from the Galaxy Zoo search has been accepted for publication. The title and abstract pretty much tell the story (the title links to the complete preprint):
William C. Keel, Anna Manning, Benne Holwerda, Massimo Mezzoprete, Chris Lintott, Kevin Schawinski, Pamela Gay, and Karen L. Masters
(PASP, likely January 2013 issue)
Analysis of galaxies with overlapping images offers a direct way to probe the distribution of dust extinction and its effects on the background light. We present a catalog of 1990 such galaxy pairs selected from the Sloan Digital Sky Survey (SDSS) by volunteers of the Galaxy Zoo project. We highlight subsamples which are particularly useful for retrieving such properties of the dust distribution as UV extinction, the extent perpendicular to the disk plane, and extinction in the inner parts of disks. The sample spans wide ranges of morphology and surface brightness, opening up the possibility of using this technique to address systematic changes in dust extinction or distribution with galaxy type. This sample will form the basis for forthcoming work on the ranges of dust distributions in local disk galaxies, both for their astrophysical implications and as the low-redshift part of a study of the evolution of dust properties. Separate lists and figures show deep overlaps, where the inner regions of the foreground galaxy are backlit, and the relatively small number of previously-known overlapping pairs outside the SDSS DR7 sky coverage.
This was the project that first drew me in to Galaxy Zoo, way back in August of 2007. Zooite’s contributions to this, perhaps the first science project organized on the Forum, exceeded my wildest hopes. As the paper shows, the previously-known set of backlit spiral galaxies in the local Universe contained only about 20, severely limiting what we could learn about the galaxies’ dust content. By the opening of Hubble Zoo, when we froze this particular list for publication, the combined catalog reached nearly 2000. Further use of this catalog is well along – we’ve had several observing runs at Kitt Peak 2.1 and 3.5m telescopes to do more detailed images, and colleague Benne Holwerda is headed to the 4.2m William Herschel Telescope atop the island of La Palma next month for more. With such a large starting sample, we can address questions we couldn’t before. How much variation in dust content and distribution do we see among apparently similar galaxies? How many dwarfish galaxies show the kind of unusual dust concentrations in their outskirts seen in one particular case? Do we see significant dust that is so cold that it eludes even far-infrared detection? On another keyboard, I’m working now to finish a paper on the ultraviolet absorption properties of dust in galaxies, combining a target list of spiral/spiral pairs from the GZ catalog with GALEX satellite data and our ground-based images. Not only is this interesting in knowing how clumpiness of dust affects its absorption properties, but is a key stepping stone toward another project – using backlit galaxies from Hubble Zoo to probe the history of dust in galaxies over cosmic time. We see some at such high redshift that the Hubble data sample light that started out well down toward the ultraviolet, so knowing how to compare that to our place and time is the basic starting point.
To show off the richness of this collection, this two-part figure from the paper shows how we divided them up into broad categories so that subsets useful for different things can be easily retrieved. This is one thing that lets us address different questions – we now have many examples of a broad range of geometry and combinations of galaxy types.
Nearly 600 Zooites contributed candidate pairs (we list the thread participants on the data page for seo services). A few deserve to be singled out. Half65, of course – not only did he find a remarkable fraction of these pairs, but he did a lot of work collecting their SDSS information. You’ll notice he’s a coauthor – fair is fair! Also, c_cld continues to display his remarkable SQL skills – he saved me a lot of time in revision by finding all the redshifts that were new when SDSS DR8 was released. Jean Tate corrected some typos in the data table (how does she do that?), and helped prod me to take the time to organize the pair members’ data more systematically by magnitude.
Regular Forum readers will recall that the first version of this paper was submitted last year. The MNRAS referees liked the analysis, but felt that the extensive catalog itself was better suited to another journal. As a result, we split that paper in two, sending the catalog and its documentation to the Publications of the Astronomical Society of the Pacific, and have been able to expand the analysis of dust distributions, so that paper will wind up even more substantial than we anticipated.
Once again – thank you to all who have taken part, and keep looking in the background as the Zoo takes in more of the sky from more telescopes!
It’s a bat! It’s a dragon! It’s a galaxy-sized set of crab claws! It’s a complex abstract design blending elements of the Mandelbrot set with classical Persian carpet design!
Or, none of the above. This is the first-cut overlay of two Hubble images of the voorwerpje-hosting AGN in UGC 11185. As usual, [O III] is in green and Hα in red; neither has yet had the contribution of starlight in the galaxy taken out. The inner set of clouds could, with a little imagination, be seen as the ind of two-sided ionization cone seen around many active galactic nuclei. But the outer cloud, the one that selected this object for our sample by extending more than 10 kiloparsecs from the core – this cloud shows pillars, loops, and gaps. (I’d like to acknowledge here the help of STScI program scientist Linda Dressel, in making suggestions for subtle changes to our pointing strategies to reduce problems from such effects as reflections from that bright star on the edge of this image).
Later the same day we first saw the Hubble images, we received additional information on UGC 11185. Colleague Alexei Moiseev (who first showed up on the GZ forum when his team was making sophisticated use of the GZ1 database to seek polar rings) has been getting data on some of these objects with the 6-meter telescope (БТА, Большой Телескоп Азимутальный or BTA) of the Russian Academy of Sciences. In the right redshift ranges, they have a Fabry-Perot device which can map the Doppler shifts of a single emission line across the whole galaxy. As supporting data, he also got this multicolor wide-field image, which shows the complicated tidal disturbances in this galaxy pair. The giant loops of stars may indicate that both are partial ring galaxies. UGC 11185 is the upper left one – you can pick out its core the bright star above it, and the glowing gas clouds around the core and to its left.
Alexei also forwarded this image of a familiar field. We’ve been re-examining the faint outer parts of IC 2497 and its companion galaxy, to see what we can learn about the history that pulled gas out where it could be ionized to form Hanny’s Voorwerp. There is a faint tidal tail to the east (left) seen in Hubble images, and now this wider-field and long-exposure BTA image show how far it stretches. Watch this space to see what we can all learn from this.
Following on the heels of the 5th anniversary of Galaxy Zoo itself, this week marks five years since Hanny pointed out the Voorwerp.
To help celebrate the occasion, we have new Hubble data on another of
its smallar relatives. This time the telescope pointed toward
SDSS J151004.01+074037.1 (SDSS 1510 for short). This has a type 2 (narrow-emission-line) AGN at z=0.0458. This was (as far as I can tell) first posted on the forum by Zooite Blackprojects, and also identified in the systematic hunt. Here it is in the SDSS:
Aa usual, these are minimally processed Hubble data, and in particular using filters where we can’t get the color right for both clouds and starlight at the same time without more work. As usual, green comes from [O III] and red from Hα , so green is more highly ionized gas. This one is cool enough already – I think of a Martian flamenco dancer with some cobwebs, but your view may vary:
Looking slightly ahead, next week, Alexei Moiseev, known on the Zoo forum from his wrk on a catalog of polar-ring galaxies based on a clever use of Zoo-1 click data, will be working with us next week, obtaining radial-velocity maps of three of these galaxies using the 6-meter Russian telescope in the Caucasus (the BTA, Bolshoi Teleskop Azimutalnyi or Large Altazimuth Telescope).
And on that note, I turn back to a new book on black-hole astrophysics,
which has me peeking ahead to page 749 for a table of timescales for
accretion phenomena. That, and wish everyone a happy, highly-ionized and just slightly late 5th Voorwerpendag!
We just got the processed Hubble images for NGC 5972. This is a galaxy with active nucleus, large double radio source, and the most extensive ionized gas we turned up in the Voorwerpje project. We knew from ground-based data that the gas is so extensive that some would fall outside the Hubble field (especially in the [O III] emission lines – for technical reasons that filter has a smaller field of view). We expected from those data that it would be spectacular. Now we have it, and the Universe once again didn’t disappoint. Another nucleus with a loop of ionized gas pushing outward (this time lined up with the giant radio source), twisted braids of gas like a 30,000-light-year double helix, and dramatically twisted filaments of dust suggesting that the galaxy still hasn’t settled down from a strong disturbance.
Here’s a combination of the Hα image (red) and [O III] (green) data, with the caution that neither has been corrected for the contribution of starlight yet. The image is about 40 arcseconds across, which translates to 75,000 light-years at the distance of NGC 5972. This gives the team plenty to mull over – for now I’ll just leave you all with this view. (Click to enlarge – you really want to.)
Our Hubble image of Voorwerpje galaxies continue to come in, and it seems each one is stranger than the last. Overnight we got our data on the Teacup system (SDSS J143029.88+133912.0). This one attracted attention through a giant emission-line loop over 16,000 light-years in diameter to one side of the nucleus.
I was worried to get email this morning that there had been a failure to lock on to one of the two needed guide stars so that the telescope might have rolled enough during the observations to compromise data quality. Inspecting the data, it looks like we’re OK. We’re OK and the galaxy is strange. This is a composite of [O III] (green) and Hα (red), right out of the software pipeline without any additional processing:
Another giant hole whose origin is obscure. The loop doesn’t even show much sign of being connected to the galaxy. The strongest [O III] does seem to trace out ionization cones, as in showing from structures near the nucleus, but that seems independent of the distribution of the gas. There are filaments in the gas that are nearly parallel, sort of like waves. Well have our work cut out for us to understand more of what’s going on here. I can hardly wait for the next one!
There was an extra treat for me with these observations. Last night, I interrupted a session with my summer class at the campus observatory to look south with binoculars and catch Hubble passing far to the southeast, no more than 13 degrees from our horizon. This was during the Hα exposure, so I saw it while it was doing these observations (it was pointed just about up in my frame of reference, as it happens). I got a picture through a 125mm telescope, showing the telescope streaking by just north of the star k Lupi. At the time, Hubble was 1600 km away over Cuba. Hubble was watching the Teacup, I was watching Hubble, and a couple of slightly puzzled students were watching me.