What Could Be Going on with Boyajian’s Star? Part X: Wrapup and Gaia’s Promise

Last time we finished up our roundup of hypotheses for Boyajian’s Star.  Let’s summarize them:

Plausible Hypotheses

• #3 Small-Scale ISM structure: This will find support if future dimmings are accompanied by increased reddening and sodium absorption.
• #4 An Intervening Bok globule: In addition to the above, this would be supported if we discover a cloud of neutral gas near Boyajian’s Star.
• #7 Comets and other circumstellar material: Plausible for the dips. Would be supported if future dips are accompanied by significant infrared flux and absorption features consistent with cometary or other circumstellar material.

Less Plausible Hypotheses

• #5 An Intervening Black Hole Disk: Would find support if we can detect the central object or if the dips repeat in reverse order, as with J1407, or if more rigorous analysis shows this to be more likely than we have estimated.

Hypotheses with Unclear Plausibility

• #2 A Solar System Cloud: Would have plausibility if such a cloud is theoretically realistic, if the cloud were found by other means, or if the dimmings are accompanied by absorption features characteristic of Solar System ices.
• #9 Alien Megastructures: Would find support if all natural hypotheses are ruled out, we detect signals, or if star suffers significant achromatic extinction.
• #13 Post-Merger Return to Normal: Would have plausibility if Boyajian’s Star is found by Gaia to be overluminous, and if simulations show this could explain the dips and dimming timescale.

Very Unlikely Hypotheses

And here’s a handy guide for what the Gaia parallax, which will determine the distance to Boyajian’s Star and is due out on September 14, will tell us:

• Within 400pc: Means that ISM extinction cannot explain current level of dimming, so favors non-ISM and non-dust explanations.  These are #9 ,11, and 12.  Could also imply that the cause is very opaque dust blocking part of the stellar disk, so #5, 6, 7, and 8 might still be OK
• Around 450pc: Means that all of the secular dimming can explained by the dust we observe along the line of sight.  Favors #2, 3, 4, 5, 6, 7,  and 8.
• Beyond 500pc: Means that the star is more luminous than we expected from the reddening.  Favors #13: return to normal brightness.
• No answer: Star does not have a good astrometric solution.  Unclear how this could happen given the lack of RV variation, but could that the 2″ companion is much bluer than we think, which would be annoying and not tell us very much except that it’s not an M dwarf, maybe boosting #5 (if it’s really the central black hole).  Might imply that there is another star nearby that we haven’t accounted for, suggesting new hypotheses.

You can vote on what you think Gaia will find here.

The paper is Wright & Sigurdsson, on the arXiv here.  Thanks for reading, and hopefully we’ll know a lot bit more in 11 days!

Update: Jason Curtis points out that the first Gaia release will not actually have the precision to distinguish among these cases!  So unless the parallax comes out really for from 450, we’ll have to wait longer than Sep. 14.

What Could Be Going on with Boyajian’s Star? Part IX: Intrinsic Variations

Last time we finished up circumstellar scenarios with a discussion of alien megastructures, the reason this star got so much press in the first place.  This installment: intrinsic variations.

I think Robin Ciardullo was the first to mention this possibility to me, though it may have been Richard Wade. The idea is that somehow the star itself is getting slowly dimmer, with occasional dips.

Hypothesis 10) Starspots and Magnetic Cycles

The most natural way stars change brightness over years and days is from stellar magnetic activity.  The Sun at the maximum part of its cycle is about 0.1% brighter than usual, and sunspots and plage coming into and out of view can also modulate its brightness by a few tenths of a percent.  More magnetically active stars might have even greater variations.

But the timescales and amplitudes are all wrong for Boyajian’s Star.  Activity cycles take decades, not centuries, and Boyajian’s Star rotates about once every 0.88 day, not many days.  If the dips were caused by spots, they should come and go every 0.88 day, but instead they last many days or longer.  Finally, in order to cause the big changes in brightness we see, the spots or cycles would have to be 10–100 times larger than the strongest effects known in other stars.

Another problem here is that Boyajian’s Star is decidedly inactive, being a hot star, not a cool star.  Unlike the Sun, it has a radiative outer layer (not a convective one), so it does not have the same dynamos that produce the Sun’s magnetic fields.  Hot stars like this have very little in the way of surface features (“stellar dermatology”) and no activity cycles (that we know of).  There are hot stars with strong magnetic fields and spots, but they are almost always slow rotators (their fields slow them down), and are generally hotter than Boyajian’s Star.

So, subjective verdict: very unlikely.

Nonetheless, something weird an unexpected is going on, so maybe we should not dismiss this entire line of reasoning entirely.  This bring us to

Hypothesis 11) Polar Spots

Montet & Simon point out that a polar spot could be doing this.  Some very cool stars are known to have large, dark, polar starspots.  This explanation nicely explains why the spots don’t come and go with a 0.88 day period: since they are at the pole, we always see them, and so at best their irregular shapes get modulated. This would explain why we see a 0.88 day photometric signature at all, on what we might expect would be a featureless star. Then, the dimmings could be due to the ebb and flow of this spot’s size and darkness on days- and century-long timescales.

Reconstruction of the surface features of the T Tauri star V410 Tauri (from Carroll et al., A&A 548, A95) shown from 4 different vantages. Note the large spot at the top pole of the star. Very young, cool stars have strong magnetic fields that seem to produce spots like this which, if the star is inclined with the spot towards us, we see persistently, with only weak rotational modulation.

This is very clever, but for the reasons I stated above we have good reasons to think this star can’t have spots like this.  (Again, if this were a thing, we should see it all the time!)  Montet & Simon offer the hypothesis very provisionally for this reason.

So my subjective verdict on this one is: not likely.

This hypothesis would find support if Gaia finds the star to be much farther away than we expect from the reddening and sodium absorption.  This would indicate that reddening is not accompanying the dimming we see, so it could be spots.  It would also find support if signs of a polar spot could be identified, such as narrow absorption features from the much cooler atmosphere, perhaps with Zeeman splitting if the spot has strong magnetic fields.

OK, what else could the star be doing?  Well, many forms of variable star are pulsating, so how about:

Hypothesis 12) Stellar Pulsations

Stars have a few characteristic timescales on which they change.  If you poke a star with a regular cadence, there are certain frequencies that will cause it to respond strongly.  Some ways this can happen are:

1. In the Sun, random convective motions cause it to “ring” with many frequencies, the strongest being around 5 minutes.  These “asteroseismic” modes are generally very, very small: they can never cause variations of order 20%, and they are usually periodic, not random like Boyajian’s Star.  The timescales are wrong for a Main Sequence star, too: these operate on sound-crossing times and their harmonics, not days or centuries.
2. Many classes of pulsating stars rely on internal instabilities involving the opacity of their constituent gasses.  If these gasses heat up, they ionize, which makes them more opaque, which makes it harder for starlight to emerge from the core to the surface, which causes the star to expand, which makes the gasses cool, which makes them recombine, which lowers their opacity, which makes it easier for starlight to emerge, which makes the star shrink, which heats the gasses… etc. etc.  These timescales can be of order days, but, like asteroseismic modes, they are periodic, not episodic, and don’t cause century-long dimming.  Delta Scuti stars are a kind of star of very similar mass and temperature to Boyajian’s Star, so it’s possible that it has something like this going on, but it’s not clear how that could cause any of the effects that we see.

Basically, all known pulsation modes are regular or semi-regular, not episodic, and none we know of operate over centuries.   If it’s some form of pulsations, it’s one we haven’t seen before or thought of before.

Subjective verdict: not likely

The last one is my favorite, from Steinn:

What if the star isn’t dimmer than it should be: what if it’s brighter, and we’re seeing it return to normal brightness?  In that case Gaia will reveal that it is much farther away than we think based on its brightness and reddening.  This would imply that the long-term “dimming” we see is the star returning to a normal state after somehow getting way too bright.

But what could that mean?  The best idea we have is some sort of merger: perhaps the star recently coalesced with another star, or a brown dwarf or planet.  This would deposit a lot of orbital and gravitational potential energy into Boyajian’s Star, which would eventually get dissipated as heat and escape as starlight, causing a temporary brightening.

It’s not clear why this would create the dips, but perhaps the merger was quite recent, and there are still hydrodynamical effects going on inside the star as the companion is “digested”, causing the internal structure of Boyajian’s Star to adjust on days-long timescales.

One issue here is that the dimming is too fast.  When confronted with big changes in energy content or flux, stars evolve on the Kelvin-Helmholz timescale, roughly the time it takes for all of the energy in the star at a given moment to finally escape the surface (while being constantly replenished by the fusion in the star’s core). For Boyajian’s Star this timescale is about 1 million years. This means that if the entire star is processing a big change in internal energy or luminosity, it takes around 1 million years to complete the adjustment.  Changing by 15% in 100 years is therefore about 10,000 times too fast.

But, the star’s radiative envelope is not very massive, so perhaps the energy never made it deep into the star? In that case the Kelvin-Helmholz timescale is a bit shorter, so maybe we’re off by only 1,000 times. It’s an order of magnitude argument, so maybe we’re being too pessimistic by a factor of 10, so we’re only off by 100 times. It’s possible that a detailed simulation of such a merger will reveal shorter timescale events, perhaps even things that might produce the dips.

So, I’m intrigued, and I like the idea despite the timescale argument not working out. It’s possible that there are other ways to temporarily brighten a star we haven’t thought of.  I’d like to hear from people who model these things before I commit to a plausibility level, so I’ll say:

Subjective verdict: unclear.

So that’s it!  That’s all I’ve got.  I’ve tried to be comprehensive, but cleverer people than me keep coming up with new ones, so I’m sure I’ve missed something.  I’m still not convinced that the right answer has appeared in the literature, but I’m hopeful that one of the explanations in our paper is correct.  Before wrapping up in the final post, though, I’d like to discuss some nonstarters that keep coming up:

Popular Nonstarters:

1. Gravity darkening.  This one got a lot of attention for some reason. Basically, stars that spin very fast have equators that are darker than their poles.  A transit or eclipse of a gravity-darkened star can therefore have an unusual shape, potentially being asymmetric.  Since some of the dips are asymmetric, some people declared the system “solved” with this suggestion.  Problem is, Boyajian’s Star is not spinning fast enough to have significant gravity-darkening, and this still doesn’t address the issues of what is causing the dips!
2. Black hole or other nearby companions.  Boyajian et al. ruled this one out, but just to reiterate their argument: Boyajian’s Star is RV stable, so it does not have any close-orbiting stellar-mass companions.  It’s not any kind of binary system.
3. Gravitational waves. I’ve heard this one suggested, presumably because they were just discovered by LIGO and so are in the zeitgeist right now.  They have no explanatory power here (i.e. there is no way they could cause what we see).
4. Asteroids in the Solar System.  We discuss Solar System solutions here.  Anything closer than the outer Solar System would not persist for years, and asteroid occultations have a very different photometric signature than Boyajian’s Star.
5. It’s an ordinary “dipper”. There are “dipper” stars that have superficially similar light curves to Boyajian’s Star. But these as caused by close-in disks and other circumstellar debris that are revealed by their long-wavelength emission, which Boyajian’s Star lacks. That was the original reason Boyajian’s Star stood out as being so weird: it’s not young, it has no disk, so it’s not a dipper. I don’t understand why this one keeps coming up.
6. Starkiller Base.  Yes, I saw The Force Awakens, too.  I presume these suggestions were all made facetiously.

OK, next time: summary of hypotheses, and what Gaia will tell us.

What Could Be Going on with Boyajian’s Star? Part VIII: Alien Megastrutures

Last time I tried to wrap up circumstellar solutions, but before moving on to intrinsic variations, it’s clear I need to address the megastruture in the room.

Hypothesis 9) Alien Megastructures

Background on this hypothesis is here, and here:

Now, I can’t give this hypothesis the treatment I’ve given the others, because, even compared to the vague, general families of solutions in the previous hypotheses, this one has very little to hang any physics on. Ancient alien civilizations could be arbitrarily advanced, and so it’s not clear what physics we’re allowed to assume. We don’t know why they would create megastructures (though energy collection seems like a good guess to me) so we have no good reason to expect any particular shape or size for them.

That said, we can build up a straw man model, and see how well it holds up.

But first, let’s dispense with some unnecessarily complicated ideas. Lintott & Simmons made me smile with their article in the Journal of Brief Ideas in which they used the timescale of secular dimming to estimate the construction time for a Dyson sphere. Similarly, Villaroel et al. skeptically mentioned this possibility in their paper.

But we don’t have to imagine building a gigantic sphere in a century to hypothesize how megastructures could explain the dimming.

Imagine that it is advantageous to collect solar energy to be used for some purpose, and that there is enough material to do so, but not an infinite supply.  Imagine that the panels have a range of sizes and orbit the star in a range of orbital periods.  In this case, the cost (in time, energy, and mass) to construct a panel is balanced by the benefit (the energy intercepted, which favors close-in panels, times the efficiency of the panels, which favors far-out panels). If too many such panels are created, the close-in ones will shadow the farther-out ones, reducing their efficiency.

In this toy model, one expects (in a rough order-of-magnitude sense) to end up with a swarm of panels that have an optical depth near 1. That is, they should not capture, say 99.999% of the photons, because the marginal efficiency of the next panel is reduced by a factor of 100,000 compared to the first one.  And they shouldn’t intercept only 0.001% of the light, because 99.999% of the light still free to take with virtually zero efficiency hit. You’d expect somewhere between, say, 10% and 90% of the light to get absorbed.

The smaller panels will appear as a translucent fluid around the star, constantly blocking some fraction between 10-90% of the light, roughly speaking. This fraction will vary as denser parts of the swarm come into and out of view, and as chance alignments of parts of the swarms at different orbital distances align. We might see variations in brightness on scales from hours to centuries. Particularly large panels—even bigger, perhaps, than the star itself—will cause large, discrete dips as they transit, with profiles according to their shape. The timescale for crossing may not be a good indicator of their distance from the star, because they might be so thin that radiation pressure is important (see the appendix here).

This is actually right in line with the observations of Boyajian’s Star: we see a constant dimming of the star, one that erratically has increased by about 15% in the past 115 years, and occasional dips.

OK, so how does the toy model hold up against long-wavelength observations?  Well, not great. The balance of efficiency with orbital distance is trickier, and interacts with the shadowing argument, but you might expect there to be a typical, characteristic temperature that is around 150K (95% maximum efficiency for a star like the Sun—we argued all of this in more detail in our paper here).

The long-wavelength constraints apply almost as well to megastructures as they do to dust. We argued in that paper that it is reasonable to expect nearly all of the energy  collected to be reradiated as waste heat.  As we saw from the long-wavelength limits, it just can’t be that 15% of the starlight is being reprocessed at 150K, or at any other temperature:

Spectral energy distribution of Boyajian’s Star, with arrows indicating upper limits. The right-most measurements are from Thompson et al. They rule out big clouds of megastructures blocking and reradiating 15% of the star’s light in all directions (black line) at 65K, because the heat would be easy to detect.  Other temperatures are actually in worse agreement with the data.

The black line is our toy model swarm blocking 15% of the light, and it is strongly inconsistent with the red upper limits from WISE and Thompson et al.

Now, there are a couple of ways out.  First, the aliens might be doing some non-dissipative work with this starlight. Perhaps they are launching interstellar probes. Perhaps they are sending out powerful laser or radio transmissions. Anything that puts all of that stellar luminosity into energy that leaves the system in a low-entropy way would reduce their waste heat luminosity.  Can that do it?

Well, if the work is all done at 65K, then the maximum (Carnot) efficiency allowed by thermodynamics is about 99%. This means that they could reduce their long-wavelength luminosity down from 15% of the star’s, to only 0.15%.  The upper limit at this temperature, as you can see in the figure above, is 0.2% (the purple line).

So… not completely ruled out, yet, but I’d have to say we’re close enough that I’d put this one down as very unlikely, even after normalizing for the unknown chance that there are megastructures there in the first place.

Another way out is that it’s not a spherical swarm. Make it an edge-on ring, and you can further reduce the waste heat. Make them radiate towards their ecliptic poles, and you can reduce it further. Turn the energy into low entropy radiation at high efficiency and do both of the above, and they’d be nigh undetectable.

So you see, the hypothesis is sufficiently flexible that it can fit almost any observations, but I do think we can say this about the vanilla, simplest, strawman scenarios:

1. IR/mm observations rule out a spherical swarm doing only dissipative work (like humanity does) being responsible for the long-term dimming
2. We can further rule out a spherical swarm sending the energy off in another way at maximum efficiency with temperatures above ~90K
3. We can lower this cut-off temperature with more sensitive measurements

So, subjective verdict: unclear, with an extra multiplier of very unlikely for the simplest spherical swarm strawman.

The megastructure hypothesis would find support if Gaia shows us that the star is actually much more extinguished than the reddening suggests (meaning there is a significant optical depth of geometric absorbers: the swarm of solar panels).  Or if, you know, we detect those radio waves that all those panels are producing!

OK, next time: back to the natural explanations, this time looking at intrinsic variability.

What Could Be Going on with Boyajian’s Star? Part VII: Circumstellar Dust

The central puzzle of Boyajian’s Star is that although the dips look a lot like those of dippers, it has no close-in disk.  That is, most stars that show this sort of behavior are young and have close-in disks, and those disks cause their dips.  Not only does Boyajian’s Star have no close-in disk, it isn’t near a star forming region, so there is no reason to think it is young, anyway.

So, if it can’t have close-in material, what could be causing the dimmings?  Well, if the material is circumstellar, it must be very cold, and/or there can’t be very much of it.  Boyajian et al. also showed that the timings and slopes of the dips also put constraints on the material’s proximity to Boyajian’s Star, meaning it needs to be pretty far-out (10 AU or so).  This brings us to:

Hypothesis 7) Comets or other circumstellar debris

Boyajian’s original hypothesis was that the dips were caused by giant swarms of giant comets.  This remains a plausible hypothesis for the dips: the comets would certainly have been warm when near periastron, but their eccentric orbits could bring them very far from the star quite quickly.  Thus, the infrared excess would only be noticeable during a dip.  If the swarm is on a long-period orbit, then we may never see them again!

On the other hand, there doesn’t seem to be any way the comets can explain the long-term dimming, especially without an infrared excess.

So, my subjective verdict on this is: plausible for the dips, very unlikely for the long-term dimming. Occum’s razor argues that if they aren’t causing the long-term dimming, then they probably aren’t causing the dips, either, but your mileage may vary on that one.

Hypothesis 8) A cool annulus of material

This is basically the hypothesis that there is a disk of material, but there is a very large (10 AU, at least) gap between the star and the inner edge of the disk (annulus).  The disk is almost, but not quite, edge-on: then, we could invoke corrugation or other irregularities that occasionally block part of the star for the dips.   This needs to be a real protoplanetary disk, not just a debris disk, because it needs to be optically thick.

There are lots of problems with this:

1. The Thompson millimeter results rule out very much mass for the disk—there is not a lot of wiggle room between what you need for the dips and the secular dimming and what would have been detected
2. I’m not aware of any theoretical justification for such ring, except maybe for young stars.
3. If the inner edge is at 10 AU, the probability of edge-on alignment is roughly 0.1%, so in order to expect to have seen one, we need to have about 1% of all Kepler stars to host such a disk (despite #2, and the fact that the field has no young stars)
4. The secular dimming is not naturally explained—if the disk is always occulting part of the star the sodium lines would probably not be symmetric, but they are.

So, while an annulus is not ruled out by the data, it doesn’t have a ton of explanatory power, and it has no theoretical justification, and it requires a very unlikely geometry and high frequency of such disks in the field.

Although I know some others still like this one a lot, these are just a bridge to far for me.  Subjective verdict: not likely.

We’ve already discussed the long-wavelength constraints that show it can’t be embedded in a cloud of material, so I won’t even mention that one.

OK, now that we’re done with all of the circumstellar possibilities, in the next installment we’ll continue our conceptual journey from Earth to the star itself and discuss intrinsic variations of the star…

Huh? What’s that? Megastructures? You want a rundown on where that hypothesis is?

Well, I hadn’t planned to talk about it, but since you asked, I suppose we could do a brief detour into some serious speculation before finishing our list.  As luck would have it I happen to have some remarks prepared right here…

All right then. Next time: alien megastructures.

What Could Be Going on with Boyajian’s Star? Part VI: Black Holes!

Last time we covered SINS and Bok globules as potential sources of the dimmings in Boyajian’s Star.  This time we’ll finish up the interstellar solutions and start to look at circumstellar solutions.

Our topic? BLACK HOLES!

Hypothesis 5) An Interstellar Black Hole Disk

Now, a very popular suggested explanation from laypeople has been “a black hole”.  For a long time, I treated this as a total non-starter: black holes are tiny, tiny, tiny, and don’t have the geometric cross-section to block any noticeable amount of light.  Further, they tend to gravitationally lens light, so if there really were a black hole between us and Boyajian’s Star we’d expect a brightening, not dimming. Finally, if it’s close enough to suck up any material, we’d see Boyajian’s Star get brighter from the accretion, we’d see light from radio to X rays from the interactions, and we’d see RV variations to boot.  So, no black hole, right?

So it’s ironic that we found another way to do it (though not what those who suggested it were thinking).  This solution is more analogous to J1407, the “planetary system under construction” discovered and characterized by Eric Mamajek and Matt Kenworthy.

Here’s the idea: the dips really suggest small-scale structure in the intervening material, but the long-term dimming suggests a smooth distribution.  One solution is a gigantic disk with annular features, like a protoplanetary disk with gaps and waves from planets and protoplanets.  The timescales involved (115 years!) mean that it must be HUGE — like 600 AU across.  What could host such a disk, but have totally escaped notice?  After all, Boyajian et al. used adaptive optics to hunt for anything nearby that could do the trick, and only found an M dwarf 2 arcseconds away.

Well, it must be very massive, and it must be dark.  Stellar remnants do the trick: a cold white dwarf, a quiescent neutron star, or a black hole.  We focus on the black hole solution in our paper.

The black hole disk from Interstellar, with the black hole’s gravity distorting the image of the disk. Our scenario is much less photogenic: the close-in disk is gone, and only a very wide, very cold disk of dust and debris remains. Also, our black hole is several solar masses, not several million.

The idea is that after a supernova explosion, there will be material that falls back towards the remnant black hole, where conservation of angular momentum requires it to collapse to a disk, and some amount of the material to move outward while a lot of it spirals in and accretes onto the black hole.  Eventually, the black hole finishes its meal, and goes quiescent, leaving behind a big inner gap within a large ring of debris outside.  This ring can now get very cold (the central object is dark! nothing to heat it), thin, and wide.  Perna et al. (2014) describe the process.

So, does it work?  Could there really be a black hole aligned with Boyajian’s Star? Well, the alignment doesn’t have to be very good: the disk needs to span a big chunk of the sky for the dimming to persist over 115 years (a couple of arcseconds, at least).  The black hole itself is small and would be unlikely to actually go between us and Boyajian’s Star (if it did it would lens it, but its Einstein radius is only ~4 mas).

We calculated the volume of space probed by Kepler for objects with that size (angle squared times typical distance cubed), multiplied by the number of stars Kepler observed, and decided you needed about 10 billion disk-bearing black holes in the Milky Way for one to have had a good chance to wonder in front of ~1 such star in the field.  That’s not too far off from the estimated number of black holes in the galaxy!

So, the numbers aren’t too bad!

I really like this one, but there still isn’t any observational evidence that such disks exist, or that they are common enough for Kepler have found one.  We haven’t done a rigorous calculation of the probabilities, so it could still fall apart upon closer inspection.

Given the uncertainties, I give it a subjective verdict of: less plausible.

This hypothesis would find support if the dips repeat in reverse order while the star starts brightening again, like J1407 did.  Alternatively, that so-called “M dwarf” 2″ away could turn out to be the central object, in an almost-but-not-totally quiescent state.  Someone get a spectrum of that thing!

Hypothesis 6) An Orbiting Black Hole Disk

I had hoped that we could make an alignment more likely by putting the black hole in orbit around Boyajian’s Star, but it turns out that makes things much harder.  In addition to the low probability of such a binary companion in the first place, the chances that it would be in a part of its orbit such that we would see it are very low, like 1 in a million low.  Since Kepler only looked at 100,000 stars, and since every star does not have such a companion, this one doesn’t work.

Subjective verdict: not likely.

OK, enough with the black holes. Next time: Circumstellar material.

Update: Commenter Herp McDerp (obviously their real name) points to this Nature article by Alastair G. W. Cameron (Bethe Prize winner and originator of the Giant Impact Hypothesis for the formation of the Moon).  In it, Cameron tries to explain the eclipses of the ε Aur system with our Hypothesis 6!  I’d write “great minds think alike” but I’m totally out of my league on this one, so I’ll just write that we’re in very good company with this hypothesis!

What Could Be Going on with Boyajian’s Star? Part V: The Interstellar Medium

Last time we covered the first two hypotheses: instrumental issues and a Solar System cloud. This time, let’s move to the interstellar medium.

Hypothesis 3) Absorption from the Interstellar Medium

Between the stars there is lots of gas and dust. The densest, coldest parts of this “interstellar medium” (ISM) form neutral gas and dust, which cause reddening, dimming, and line absorption in stars. For instance, all evidence points to Boyajian’s Star having its light pass through enough dust and neutral gas on the way to Earth to make it about 35% dimmer at visible wavelengths than it would be without that stuff in the way. This is expected for any star in its part of the Galaxy.

But, one asks, maybe there are some especially dense pockets along that our line of sight occasionally sweeps past? I had always rejected this line of thought because if that were a thing, all sorts of stars would do that. After all, Kepler looked at over 100,000 other stars and none of them ever showed this behavior.

Carl Heiles, radio astronomer extraordinaire, and my wife’s thesis adviser at UC Berkeley. He has done a lot of work on “tiny scale atomic structure” in the ISM, among many other topics.

But, it turns out rare dense patches are a thing! I was at Berkeley recently and chatted with Carl Heiles, and he pointed me to SINS — small ionized and neutral structures in the diffuse interstellar medium. He was actually one of the folks who first brought these things to the attention of the broader community and postulated that they are short-lived, overdense, corrugated sheets and/or filaments in the ISM, and that when our line of sight aligns with a tangent point of such a structure we get a temporary jump in absorption.

So it turns out that this is a whole field—Carl pointed me to this conference on the topic 10 years ago. So, could this be the answer? Well, one problem is that the columns and sizes implied by Boyajian’s Star are much different from the “tiny scale atomic structure” that Carl describes. Those structures are typically around 30 AU across and block maybe 0.1% of the visible light that passes through them.  We need about 100 times as much dust, and we need structures maybe 100–1000 times smaller than that.

But, it’s not clear that we would know about such structures if they did exist—you would basically need to launch Kepler to notice them. The ones they know about are pretty rare (most sources don’t show any evidence for them) so regions this dense and small could be so rare that Boyajian’s Star is the only one that sees them.

So, if we hypothesize that there is a spectrum of these SINS down to even smaller scales than have previously been seen, and that these smaller structures have even higher densities, and if these extensions persist across 2-3 orders of magnitude, then we would expect to very occasionally see stars behave like Boyajian’s Star!

This hypothesis is supported by the fact that the existing dimming implied by the ISM reddening and sodium absorption is enough to explain all of the Schaefer and Montet & Simon dimming — they see 15% or so, and the ISM is causing over twice that.  This hypothesis would find support if during a future dip (or if the star’s long-term brightness continues to change a lot, in either direction) we see a corresponding change in the reddening, and in the sodium absorption features.

I like this one.  Subjective verdict: plausible!

Hypothesis 4) Absorption from an Interstellar Molecular Cloud

Barnard 335, a good example of a small, isolated molecular cloud—or “Bok globule”—and the subject of my undergraduate thesis with Prof. Dan Clemens at Boston University. Source: https://forum.cosmoquest.org/showthread.php?149935-Barnard-335

A more obvious way to make a star dimmer is with an interstellar molecular cloud.  We don’t expect to see any of these up in the direction of Boyajian’s Star, but such high latitude clouds do exist.  Now, normally such clouds are obvious because they are the site of star formation, and young, forming stars light the cloud up at wavelengths from the radio to X rays.  But some are quiescent, and if a star were not forming in the cloud it might not be obvious.

Now, such quiescent clouds are usually obvious because they are big (or part of a bigger cloud complex). There are small, isolated ones, though, called Bok globules, and they are usually found because they block a lot of starlight, so you see what looks like a big hole in the sky where stars should be.

At least, you do when they’re big and in front of a rich star field, like in the Galactic Plane. If they’re small and farther away, they can be pretty small, and if the background star density is low, you might miss them entirely.  If there were a small (0.1 AU) Bok globule in front of Boyajian’s Star about 300 pc away, I don’t think it would have been noticed before.

Bok globules have smoothly varying densities, so a varying line of sight through it would naturally explain the long-term dimming.  The dips would imply that this Bok globule has dense, sub-AU knots within it that our line of sight is probing.  That’s a bit of a stretch, but, hey, if SINS exist in the diffuse ISM, why not in a dense cloud?

This hypothesis would find support if we could find the cloud, perhaps with a gas map done by the VLA or something.  Even a single-dish radio telescope might at least spot some molecular gas in that general direction compared to neighboring direction, which would lend this hypothesis support.

This one isn’t quite as nice as SINS for me, but I still think it’s got a lot going for it.  Subjective verdict: plausible!

OK, enough words.  Next time: our final interstellar hypothesis, and then we’ll get in close and take a look at the possibilities for material in orbit around Boyajian’s Star!

What Could Be Going on with Boyajian’s Star? Part IV: Nearby Stars, Instrumental Effects, and a Solar System Cloud

Last time, we discussed the periodicities (or lack thereof) in the dips of Boyajian’s Star, and the implications of the sodium absorption and reddening we see.  The last piece of observational evidence I’d like to introduce is whether any neighboring stars are variable.  After all, if there is a large cloud between us and Boyajian’s Star, it should block light from other stars, too.

Photometry of Nearby Stars

Well, there is a star, KIC 8462860, which sits 25′′ NNW of Boyajian’s Star.  It doesn’t have the same sort of time-series as Boyajian’s Star, so we can’t look for dips, but Ben Montet did extract its long-term light curve from the Kepler full-frame imagery, and he graciously gave them to me for publication:

Photometry of KIC 8462860, a star 25′′ NNW of Boyajian’s Star, kindly provided by Ben Montet, using the same methods he and Josh Simon used to find the long-term dimming of Boyajian’s Star. Nothing to see here, apparently.

Nothing to see here, apparently—this looks like an ordinary constant star, like most of the >200 others Montet & Simon looked at.  Nonetheless, Steinn and I strongly encourage photometry monitoring of all stars within 1′ of Boyajian’s Star, just in case.

OK, so that’s going to help with explanations invoking a cloud of material. Now on to the hypotheses!

Hypothesis 1) It’s Instrumental

That is, there is no dimming to explain, it’s an artifact of the instruments.  Dr. Boyajian ruled this out in her paper regarding the dips, and since then many groups have gone back to the Kepler data to see if they can find a problem, including Kepler team members.  The dips are real.

The long-term dimming Schaefer sees could be instrumental — indeed there was a big food-fight over this issue, but, as I wrote in Part I, the Montet & Simon discovery of similar dimming during the Kepler mission (and careful use of control stars) provides independent confirmation of the phenomenon.

I think we can put this one to bed.  Subjective verdict: very unlikely

Hypothesis 2) A Solar System Cloud

Could there be a cloud of — something — in the Solar System blocking light from Boyajian’s Star?  Let’s set aside where it came from for now—does the hypothesis have explanatory power?

The Earth, Kepler, the Sun, and Boyajian’s Star are all moving.  The motion of the star is called its space motion and the apparent change in position of the star due to its motion and the Sun’s is called the star’s proper motion.  If there is something between us and the star, then proper motion should change our line of sight through it.  Kepler also moves around the Sun, and that results in an apparent, annual elliptical motion across the sky we call parallax.  Nearby stuff seems to move due to parallax much more than background stars, so if there is a Solar System cloud, then we would expect our line of sight to trace an annual ellipse through it, in addition to a slow drift due to proper motion.

For the moment, let’s put the hypothetical cloud out at 10,000 AU.  Parallax would make it appear to move by about 20 arcseconds, and its orbital motion would move it by about the same amount over 100 years.  So if the cloud is 20″ across, it could be responsible for the long-term dimming.  This would also help explain the 1.96 Kepler year gap between the two dips (although not the lack of dips at 0.98 years): that’s the time it takes our line of sight from Kepler to return to about the same place, with ~1% taken off due to the cloud’s own orbital motion.

So, in this scenario the long-term dimming is just a density gradient in the cloud, and the dips are from dense knots in the cloud that we briefly look through when Kepler and Boyajian’s Star line up just so.

So, what are the problems?  Well for one thing, the density gradient doesn’t seem modulated on an annual timescale.  For another, the sodium lines in the spectrum don’t seem to be at zero velocity with respect to the Solar System barycenter.  Finally, why would there be a cloud of dust out there?  Not only is Boyajian’s Star way above the ecliptic (but does that even matter at 10,000 AU?), but a 20″ cloud at 10,000 AU would be 1 AU across.  What could cause it?

Steinn likes the idea of a very low-velocity cometary collision that kicked up ice and dust in a big cloud.  It wouldn’t take much mass to hold the dust in a Hill sphere 1AU across (an asteroid would do it).  I prefer a big KBO-type object with a very gentle geyser that burps out dense plumes occasionally.

If we see another dip, and the spectrum of Boyajian’s Star shows evidence of Solar System ices in absorption then, I think this idea might gain traction.

Nonetheless, the combination of a highly speculative cloud, a missing annual timescale, no obvious dimming of neighbor stars, and no clear sodium absorption feature cause me to give a subjective rating of unclear to this one.  That is, I’ll need some outer Solar System people to weigh in on likelihoods before I give it a grade.

Credit Where Credit Is Due

I should take this opportunity to note that many of these hypotheses are not original to Steinn and me.  Many have been suggested independently to us privately, both in person and over email, at Q&A sessions after talks, in social media, and among our professional colleagues.  If in this or future installments you recognize an idea as one you pitched to me, let me say:

1. Thanks for your suggestion; it helped me think about the problem
2. You weren’t the only one to suggest it, and you probably weren’t the first
3. I’m sorry if you are not in our acknowledgements section; we could not acknowledge everybody or track down every suggestion, but even so our original acknowledgements were so extensive that the editor asked us to scale them back (Letters are supposed to be short).

What Could Be Going on with Boyajian’s Star? Part III: Periodic(?) Dips and Interstellar(?) Sodium

Last time, I looked at the infrared constraints on solutions to the puzzle of Boyajian’s Star.  This time, let’s look at other constraints.

Boyajian and others have noted that the deepest dips seem to have some patterns to them.

A 2 year period?

For instance, two of the deepest dips occur 2.000 years apart, which is an awfully precise number to be mere coincidence.

But, coincidence it is: remember that Kepler does not orbit the Earth, it orbits the Sun, and it does so in an Earth-trailing orbit, meaning that it has a different orbital period than the Earth!  So the relevant year is not an Earth year, but a Kepler year.  This makes those two dips’ interval less suspiciously precise: they are 1.96 Kepler years apart.  Also, if the Kepler orbit were responsible for those two dips, then one would also expect to have seen dips 0.98 Kepler years before and after the first of those—and we don’t.

A 48.4 day period?

Another suspicious bit of timing is that many of the deepest dips seem to occur with an interval of 24.2 days.  Boyajian noted that this looks like a 48.4 day orbital period, in which something luminous blocks the star every 48.4 days, and is itself blocked half a cycle later as it goes behind Boyajian’s Star.

I think it was Mark Conde who first pointed out to me that this was probably a coincidence.  I redid the calculation myself, and asked: if the dip times were perfectly random, how often would we be able to find a similarly strong coincidence?  I drew six times of dips randomly 10,000 times and hunted for periods that lined up at least as well as the 24.2 day coincidences in the timings of the six actual dips in the Kepler data.  Over 15% of the time, I found better coincidences, and among all of the best coincidences I found, the median period was 20.8 days.

It other words, with only 6 dips, it’s quite common to see phantom periodicities if you check enough periods.  True, these are a bit better lined up than random, but that’s probably why they were noticed and I did this analysis in the first place.

So, I don’t think there is any reason to suspect that the dips are periodic. That doesn’t mean they’re not, just that we should not feel constrained by any periodicities when looking for solutions to the puzzle.

Sodium absorption and reddening

Boyajian’s Star’s sodium lines are very broad because the star is rotating rapidly. Between us and the star, there are clouds of neutral gas, and this gas contains sodium and dust (and lots of other stuff).  As a result, the dust makes the star a bit too faint in the bluer wavelengths, and the sodium absorbs light at its characteristic wavelengths near 590 nm.  This is not unusual: at the nominal distance of Boyajian’s Star (450 pc) we expect there to be plenty of this interstellar material.

The reddening from dust makes the blue wavelengths about 10% fainter than it should be compared to green-ish wavelengths (we write E(B-V) = 0.1).  This also implies that about 35% of all of the visible light from the star in our direction is attenuated by dust before it reaches Earth.

We can also use the sodium lines to “find” the source of this dust, presuming that the sodium and the dust go together (a reasonable but imprecise assumption).  Here is what the sodium lines look like, (analysis courtesy of (newly-minted-PhD) Jason Curtis, Keck/HIRES spectrum courtesy of B.J. Fulton and Andrew Howard):

Boyajian’s Star’s sodium line. The big “bowl” is the star’s absorption line, broadened by its rotation. The narrow features are due to intervening sodium gas.

The narrow sodium features, modeled as absorption from three clouds of sodium between us and Boyajian’s Star by Jason Curtis.

The total sodium absorption we see (420 mÅ for the experts) translates to roughly E(B-V)=0.1, which is exactly what we see, so it all hangs together: at the time of these observations (2015) the sodium between us and Boyajian’s Star an the reddening were consistent.

This has implications for the long-term dimming seen by Shaefer and Montet & Simon: if it is due to dust and neutral gas, then these clouds are the ones responsible.  Note that none of the lines are centered on Boyajian’s Star’s line: this means they have significant line-of-sight motion with respect to Boyajian’s Star, making it unlikely (I would argue) that they are in clouds orbiting the star.  The RV of Boyajian’s Star is +4 km/s, and the red-most cloud is offset by ~10 km/s, so it has ~5 km/s motion with respect to the solar system barycenter.  This all argues to me that the clouds are what they appear to be and what we would guess they would be if Boyajian’s Star were not so weird: ordinary gas and dust in the interstellar medium.

Next time: what are the stars near Boyajain’s Star doing? Then, on to the hypotheses!

What Could Be Going on with Boyajian’s Star? Part II: Long-Wavelength Constraints

Last time, I laid out the background for Boyajian’s Star.  Let’s look at some of the observational constraints on families of possible solutions.

First, there’s the lack of infrared excess. This actually is the main reason Boyajian’s Star is weird. Other stars, like this “dipper”, behave similarly to Boyajian’s Star but have whopping infrared excesses. That is, there is a lot of extra infrared light in excess of what you would expect from a “naked” star. This is because there is a lot of circumstellar material around those stars in the form of a disk, and parts of that disk sometimes occult the star, causing big drops in brightness. In those cases there is some puzzle in the exact geometry of the situation, but there is no mystery regarding what’s causing the dips.

With Boyajian’s Star, the lack of infrared excess is very puzzling in the context of its dips.  If something is blocking the starlight, why is there no infrared light coming from it?  Massimo Marengo and Casey Lisse published papers recently showing that the lack of IR excess in archival data is also a lack of IR excess today, using recent Spitzer and IRTF data. This rules out many categories of solutions where all the circumstellar dust formed recently due to a planetary collision (for instance).

More recently, Thompson et al. showed that there is no detectable millimeter flux from Boyajian’s Star.  This upper limit is weaker, but rules out cooler dust.  Specifically, they claim there can be no more than 7.7 Earth masses of dust within 200 AU, and no more than about 10-3 Earth masses of dust at the orbital distances implied by the durations of the dips.  This rules out some origins for the long-term secular dimming seen by Schaefer: there can’t be a cloud of stuff around the star constantly blocking 15% of the light, or it would certainly intercept and reradiate more light than we see.  Here’s what I mean:

Red points showing the spectral energy distribution of Boyajian’s Star, with arrows indicating upper limits. The right-most measurements are from Thompson et al. They rule out big clouds of 65K dust blocking more than 0.2% of the star’s light in all directions, because the dust would reradiate at levels easy to detect.  The two curves are models consistent with the short-wavelength data and differing only in the fraction of starlight being intercepted and re-radiated as heat.

In this figure, you can see the optical spectrum of the star on the left, with the red points being the measured brightnesses.  It follows a normal curve for a star.  Disks of the sort that cause the “dippers” are firmly ruled out: they have hot, close-in dust that have lots of emission at 5-20 microns, which we don’t see in the red points.

The black line is actually a model of the star that matches the detailed spectrum we really see 20 microns and shorter.  Longward of 10 microns, there are two curves: the black curve is what you would see if the star were surrounded by a cloud of dust absorbing 15% of its light.  I chose 15% because that is the total amount of dimming seen by Shaefer and Montet & Simon.  The red arrows are upper limits: the star is dimmer than that at those wavelengths. Clearly, the long-term dimming can’t be created by such a cloud, or the dust would be warm enough to be seen by Thompson at 1 mm ( =1000 microns).  You can’t save the hypothesis by making the dust colder, either, because that just moves the curve to the right.

In fact, if there is warm-ish dust aroud the star, it cannot be blocking more than 0.2% of the starlight (the purple curve), and even then it only squeezes between the existing upper limits if it’s at 65K, which is pretty cold.  This constrains possible solutions to the long-term dimming.

Now, if the dust is in an edge-on ring, then it could absorb only 0.1% (or less) of the starlight in total, but still block 15% along our line of sight. In that case, it would not be seen by the current observations, as long as it was cold enough.  So: disks and clouds are out, but rings (and comets) are still allowed by the IR and mm observations.

Ok, that’s enough words for one post.  Next time: If the long-term dimming is going on right now, shouldn’t we be able to determine its composition from absorption features in the star’s spectrum?  Also, aren’t the dips periodic, and can we predict the next one?

What Could Be Going on with Boyajian’s Star? Part I

I’ve just re-submitted a paper, which I expect to be accepted soon in light of a very favorable and constructive referee’s report, about KIC 8462852.  It covers the puzzle as I see it now, the landscape of solutions—from the plausible to the all-but-impossible—and opportunities for future progress. I’m especially excited for the GAIA parallax, which will really help us to narrow things down!

So I’m going to slow-blog the paper over the next week or so, up until the day it actually appears on the arXiv (after it’s accepted).

OK, let’s go!

The Story So Far

Dr. Tabetha Boyajian (now an assistant professor at LSU) first announced KIC 8462852 to the world in a paper that described how it was discovered, how it is an apparently ordinary F star except for its bizarre series of photometric “dips,” and how hard she and her co-authors, including Prof. Saul Rappaport, worked to solve the puzzle.  I’ve blogged previously about the whole story, including the subsequent media coverage here, and you should read that to catch up if you’re not familiar with the star.  I also gave a talk about it that you can watch here:

Then Bradley Schaefer looked at old DASCH photometry and found that Boyajian’s Star has been fading over the past 100 years, a claim at least as extraordinary as the star’s Kepler light curve.  There was a lot of shouting over this claim, and whether it was right, which Kimberly Cartier and I documented in an article for the Atlantic, linked in this blog post.

Ben Montet, looking up, presumably at Boyajian’s Star.

The big news recently is that Ben Montet & Josh Simon very cleverly recently used the Kepler full-frame imagery—some calibration data that doesn’t get much attention because you can’t use it to find planets—to get accurate long-term photometry of Boyajian’s Star over the course of the mission.  Amazingly (to everyone but Bradley, I suspect), they found that the star got 4% dimmer over 4 years, in a monotonic but irregular way.  What’s more it is the only star out of > 200 that show this effect.

In my opinion, this independent confirmation of the unprecedented effect Schaefer claimed—even if not covering the same time period—shows that Shaefer’s analysis is correct and the star really has dimmed a lot.  Adding the two effects, the star is now apparently at least 17% dimmer than it was in 1890!

Where We Are Now

So what the heck is going on?  We now have two inexplicable things going on: long-term, secular dimming of 17% in 115 years, and these days-long, deep “dips” of up to 22%.  Both are very hard to explain.

Well, Occum’s Razor points towards a single explanation for both the secular dimming and the dips. Of course, in principle they may be unrelated, in which case Boyajian’s Star is extraordinary for two independent reasons. But I favor explanations that could plausibly cause both.  At any rate, I’ve been engaging in a lot of “clean-sheet” reasoning lately, trying to cover all of the bases, and working with a lot of people to figure out what’s plausible.  Steinn Sigurdsson, my often-time theorist sounding-board, is a co-author.

We decided that the explanation for the dimming must occur either at Boyajian’s Star itself (intrinsic variability), in orbit around it (circumstellar material), between the Sun and Boyajian’s Star (interstellar material) or in the Solar System (either between us and the star or in our instruments).  In future installments, I’ll cover the observational constraints, including dip periodicities, long-wavelength constraints, and the brightnesses of nearby stars, and then go through each possibility and give it a plausibility.

Wait, What Did You Call the Star?

Prof. Boyajian, looking up, presumably at Boyajian’s Star.

I’ve decided to call it “Boyajian’s Star“.  Prof. Boyajian herself calls it the “WTF” star, ostensibly after the subtitle of her paper (“Where’s the Flux?”, natch).  Early on during the media firestorm, a reporter asked me what I call it, and I admitted I could never remember its phone number and that within my group we called it “Tabby’s Star,”  because she first showed it to us, back before it was published. The name stuck, and now that’s what it’s usually called.

I’m conflicted about that term.  On the one hand, it has ensured that Tabby gets the credit for her work establishing how strange the star is, which is great (I wish I could claim that’s why I first used the term! It’s certainly why I kept using it).  On the other hand, that name is actually the most common among professional astronomers, which is incongruous with other eponymous stars.  You see, there’s a long tradition of naming stars after the people who made them famous—Barnard’s Star, Kapteyn’s Star, Przybylski’s Star—but professionalism and formality dictate that we always use the namesake’s surname.  Not only does “Tabby’s Star” use her given name, it uses the diminutive form.  It reminds me too much of one of the sexist double-standards common in academia (e.g. a man is “Prof. Smith”, but a woman is “Jenny”, especially from undergraduates!)

So, I’ve decided that when it comes to the professional literature, I’ll follow tradition and call it “Boyajian’s Star”.  If other astronomers do the same, perhaps it will stick.

The paper is Wright & Sigurdsson, “Families of Plausible Solutions to the Puzzle of Boyajian’s Star,” and I’ll dribble out more about it in future installments until the arXiv posting.

Part II is here.

Update: By popular demand, Tabby has given us a pronunciation guide for “Boyajian”. She says “boy-AH-zhun”, with the j sounding like that in “Jean-Luc Picard” (that is, say “sh,” but use your voice, don’t whisper).

Giant Planets Transiting Subgiants

It’s been a while since I’ve discussed the subgiant mass issue, but there’s a nifty new paper out that gives me occasion to revisit it (original controversy, our response, another mention here). The basic outline is that there is a mild controversy over the masses of subgiant stars — stars transitioning between their long Main Sequence lives and their final, giant phase before they run out of nuclear fuel. John Johnson studied subgiants that were between 1.5-2 solar masses back when they were on the Main Sequence (“Retired A Stars”) to show that they are more likely to have giant planets detected around them than stars of the Sun’s mass or lower. Jamie Lloyd at Cornell thinks these are really mostly just solar-mass stars, because there shouldn’t be very many retired A stars (it’s a short phase of a rare kind of star). After refereeing the discussion between my friends for a while, I finally sided with John.

Since then, Luan Ghezzi and John have a nice paper where they look at all of the subgiants with known masses and find that there is no reason to doubt their mass estimates.

But what we’ve really wanted to have is a transiting planet around a subgiant. Transiting planets provide a way to estimate the density of a star completely independently of other methods, which, combined with even a rough radius estimate, would allow a subgiant’s mass to be independently estimated.

The problems are many: subgiants don’t have a lot of close-in planets, they’re big, so the transiting planets have very small depths, and they’re big, so the transits are looooooong.

Prof. Josh Pepper of Lehigh University.

Well, the KELT team has found one, and around a bright subgiant!  Josh Pepper leads the team that just announced KELT-11 b, an inflated  0.2 Jupiter mass giant orbiting a V=8 star.   KELT is the “Kilodegree Extremely Little Telescope” array, designed to scan huge swaths of sky for transiting planets. Its architects include Thomas Beatty of Penn State, Jason Eastman now at Harvard, and Scott Gaudi at Ohio State, to name a few of those I’ve worked closely with.

KELT-11 is brightest star known to host a transiting planet in the southern hemisphere!  The paper has a ton of authors because a big team of people worked really hard to get this star characterized. I’m involved because MINERVA contributed some photometry (fourth curve in figure 2) to try to nail this thing down.

Because it’s a subgiant, the signal is very weak, and very long.  The transit is eight hours long, which means that virtually no single telescope on Earth can get the whole transit in one night (we don’t have any south pole photometers!).  As a result, it’s challenging to remove systematics from ground-based observing: you never see both ingress and egress with the same data set.

A precise mass from the transit alone will still need to wait for space-based data that can get the entire transit in one go, but in the paper the team uses several independent methods to estimate the mass, including their best estimate from the light curve.  In section 3.8, four different estimates are used and all four find a mass > 1.3 solar masses, with the right answer probably around 1.4. This further confirms the methodologies John uses to estimate masses, giving more evidence to the assertion that the subgiants in his sample really are “Retired A Stars”.

It’s a great paper about a superlative planetary system ripe for extensive followup.  You can find it on the arXiv now here:

KELT-11b: A Highly Inflated Sub-Saturn Exoplanet Transiting the V=8 Subgiant HD 93396

We report the discovery of a transiting exoplanet, KELT-11b, orbiting the bright (V=8.0) subgiant HD 93396. A global analysis of the system shows that the host star is an evolved subgiant star with Teff=5370±51 K, M=1.438+0.0610.052M, R=2.72+0.210.17R, log g=3.727+0.0400.046, and [Fe/H]=0.180±0.075. The planet is a low-mass gas giant in a P=4.736529±0.00006 day orbit, with MP=0.195±0.018MJ, RP=1.37+0.150.12RJ, ρP=0.093+0.0280.024 g cm3, surface gravity log gP=2.407+0.0800.086, and equilibrium temperature Teq=1712+5146 K. KELT-11 is the brightest known transiting exoplanet host in the southern hemisphere by more than a magnitude, and is the 6th brightest transit host to date. The planet is one of the most inflated planets known, with an exceptionally large atmospheric scale height (2763 km), and an associated size of the expected atmospheric transmission signal of 5.6%. These attributes make the KELT-11 system a valuable target for follow-up and atmospheric characterization, and it promises to become one of the benchmark systems for the study of inflated exoplanets.

 Comments: 15 pages, Submitted to AAS Journals Subjects: Earth and Planetary Astrophysics (astro-ph.EP) Cite as: arXiv:1607.01755 [astro-ph.EP] (or arXiv:1607.01755v1 [astro-ph.EP] for this version)

Three New Neptunes

One of my looooooooooooong term projects is monitoring the bright stars in the sky for yet more exoplanets.

These bright stars are some of the very closest Sun-like stars in the sky, and primary targets for next-generation efforts like MINERVA and NEID.  Because of their proximity, their planets are the most easily imaged cold planets, the most easily weighed by astrometric measurement (someday), and (even further in the future) the only ones humanity can plausibly target with interstellar probes. We will study these systems for as long as we pursue astronomy.

PSU Professor Eric Ford (but I knew him before he was famous, back in our Berkeley days)

For a few years Eric Ford and I routinely submitted proposals to NExScI to continue monitoring these stars at Keck, and for a while we were successful. It’s a hard sell to a competitive TAC, though, and once Kepler targets started (deservedly) getting lots of NASA Keck RV time, it didn’t make sense to keep proposing.

While it’s not as quick and flashy as Kepler science can be, there are three big ways this sort of patient astronomy pays off: finally getting orbits for long period planets (as in this paper by my student Katherina Feng), monitoring planet-planet interactions among known exoplanets (as in this paper by Ben Nelson), and getting enough data to find new low-mass planets orbiting these stars.

BJ Fulton, University of Hawaii graduate student and author of a nice new paper on some familiar systems.

Well, a lot of that Keck time we invested (combined with a lot of UC and Hawaii Keck time, plus APF time) has paid off yet again. BJ Fulton, a graduate student at Hawaii with Andrew Howard, has just posted his latest paper announcing three Neptune-massed planets orbiting bright, nearby stars.  There’s a lot in here!

First, HD 42618: it’s a solar analog (1.05 solar masses) at 24 pc that undergoes a magnetic activity cycle (something we can detect when we monitor stars for decades!  It also helps to have Greg Henry’s photometry for this.) There’s CoRoT photometry, so the team was able to extract asteroseismic information to confirm the stellar parameters. The new planet orbits near 0.5 AU, and receives 3x Earth’s insolation from its star.  Interestingly, BJ had to remove the stellar activity cycle from the RV time series to get to the planet: the amplitude of the effect is 3 m/s.  That’s not abnormally high, but high enough to be annoying.  There is also a signal at 2 m/s and P=388 days: this is close enough to 365 days to be both suspicious and difficult to check; if due to another planet, that one is at least 22 Earth masses.

Next up: HD 164922, a G9 star a 22 pc.  Here, interferometrists were able to actually determine the radius of the star directly, greatly improving our stellar parameter estimates. Back when I published the Catalog of Nearby Exoplanets, we included in that paper the announcement of HD 164922 b, a P=3-year giant planet. In 2007, as part of my thesis I published a paper in which we noted that we saw a hint of a low amplitude second planet:

— HD 164922 has a known planet with a 3.1 y orbital period. For this star, the FAP
for a second planet is <1%. The best fit for this second planet has P = 75.8 d and
m sin i = 0.06 MJup. The amplitude of this signal is extremely low — only K = 3 m/s —
making this an intriguing but marginal detection.

As luck would have it, this signal was real! BJ finds P=75.8d and K=2.2 m/s — no wonder we had such a hard time picking it out back in 2007!  What a difference 9 years of concentrated RV work makes.

The last one is ρ CrB (HD 143761), a V=5 G0 star only 17 pc away.  The first planet around this star was detected back in almost 20 years ago (Noyes et al. 1997!) — one of the very first exoplanets.  This was back when there was a lot of discussion (too much, in fact) about some or all of the detected exoplanets being face-on stellar binaries.  More than once, astronomers pointed to astrometric data suggesting that the signal Noyes et al. saw was from a face-on brown dwarf or stellar companion. Now, this in itself was really interesting, because brown dwarfs were only known for about 2 years when ρ CrB b was discovered!  But not as interesting as exoplanets.

Well, not only do we not see any evidence of a stellar companion in interferometry or speckle imaging, but BJ has found a second planet in the system, and he shows that stability constraints make it very unlikely that there is a big old brown dwarf down there — ρ CrB b is almost certainly a planet.

Seeing these planets published is so rewarding—an example of literally decades of work coming to fruition. Seeing these old systems again is sometimes like seeing old friends after a long time and meeting their young families.

You can find the full paper on the arXiv here.  You can email BJ with questions or complements about the paper here.

Right on Red

A traffic issue has vexed me for years, and we finally got to the bottom of it.

There are two signs in Pennsylvania that have always made me nervous to turn right at a red light: “stop here on red” and “right turn signal”.

Here they both are at the corner of East Branch Road and South Atherton street near my house:

This is the Google Streetview view from the right-turn only lane.  The sign on the right is pretty clear: on a red light you stop there, at that line.  BUT… is there an implication that you must stay stopped until the light turns green? I always assumed no, but couldn’t be sure.  Is the sign merely telling motorists where they must stop when they do for a red light, or is it an imperative to remain stopped? A case could be made either way, and presumably traffic law settled the question long ago.

Then there’s the second sign by the lights.  Here’s a better view of it:

This one also seems pretty clear: the two lights on the right of this five-light signal are for people turning right. Indeed, in states where lights are shaped like arrows instead of circles, there is no need for such a sign.

BUT…does that mean that if I want to make a right turn, I have to obey that signal, thus negating the usual right-on-red rule? After all, in states with arrow-shaped lights for right turners, there is also a red arrow. If this sign thus turns circles into arrows, then right turners must remain stopped until the right green light is activated. Or does the sign only refer to the yellow and green light, not the shared red?  In that case, there is no red light for right turners!  The case for no right on red here is actually pretty strong, but still ambiguous.

Either sign alone, and I would take the right turn without too much worry.  But together, these two signs always made me worry that a police car would catch me turning right on red and ticket me.  Friends had told stories about how other friends had gotten tickets for rights on red when one of these signs was present, but I assumed that was somehow from some more complex or distinguished case.

Well, a discussion with friends finally got me to do some research online, while my wife Julia just did the right thing, calling the police to ask.

I found this, which reads authoritatively on the subject:

Also, the PA drivers’ manual says nothing about such a sign that would prohibit right on red:
https://www.dot.state.pa.us/Public/DVSPubsForms/BDL/BDL%20Manuals/Manuals/PA%20Drivers%20Manual%20By%20Chapter/English/chapter_2.pdf

Less authoritatively, every forum I can find online agrees that right on red with the “right turn signal” sign is allowed. For instance:
http://travel.stackexchange.com/questions/24603/right-turn-signal-in-pennsylvania-can-i-turn-on-red

To top it off, Julia reports that the State College police department gets these questions all the time.  The bottom line:

Neither sign implies that you cannot turn right on red.  The only sign that prohibits otherwise legal rights on red is this one:

You’re welcome.

Next time on AstroWright: Traffic Detective: at how many intersections will one person have the opportunity to legally execute a left-on-red in a lifetime?

Citizen Science

Can citizen science include Kickstarter-like campaigns for certain projects?

It’s a fascinating proposition. Success rates for NSF and NASA grants are below 20% (and in some cases, below 10%), meaning that even outstanding, high-impact, low-lisk research has a low chance of getting funded. Sites like experiment.com have offered scientists ways to fund their research using a Kickstarter model: ask the public to pitch in.

For this to work, a project needs to capture the public’s attention. KIC 8462852 certainly has, and after a lot f recommendations on the topic, Tabetha Boyajian decided to start a Kickstarter campaign to fund follow-up observations of it.

Things started slowly, but the effort has really picked up steam in the past 48 hours.  We have a Cool Worlds video about it, courtesy of David Kipping:

and I was asked to mention it at my recent panel discussion on SETI at the New York Academy of Sciences:

I think it would be fascinating to see if $100,000 projects could be funded this way—in this era of incredibly tight funding landscapes, it’s clear that there’s an appetite for more (and different) science than the government funds. I would not advocate that we move over to such a model entirely of course—peer reviewed proposal are still the best way to move science ahead, especially in directions with merits that are difficult to explain in lay terms—but it’s something that seems to be getting more popular. Will get get to$100,000?  Well, as I write this we’re at \$92,000 and there’s 24 hours to go.  We’re achingly close.

Give us a hand, will you?

The logo for Tabetha Boyajian’s Kickstarter campaign.

Effects of a Young Sun on a Young Earth

I’m pleased to announce three out-of-cycle opportunities to work with Penn State astronomers — including me! — through the NASA Nexus for Exoplanet System Science.  This cross-disciplinary research network is soliciting applications due July 1 for Nasa Postdoctoral Program fellows to come to Penn State to work on projects that cross disciplines and NExSS teams. I’ll describe the two with me in these blog posts; the third is to work with Eric Ford on the statistical properties of exoplanets (read the ad!)

The first opportunity is at this link.  Here is the second opportunity to work with me:

Effects of a Young Sun on a Young Earth

There is a huge controversy in heliophysics/stellar astrophysics over the composition of the Sun.  This might be surprising, given how well we (think) we understand the patterns of abundances in the Solar System, and how well we can study the Sun’s photosphere, but it turns out there’s a fly in the ointment.

The Standard Solar Model has been a high point in stellar astrophysics for decades.  Helioseismology provides data that confirms the model to very high precision, with a tiny disagreement at the base of the convective zone, where the physics gets tricky and uncertain.  This model includes a detailed map of the abundances of the elements as a function of depth in the Sun.

Martin Asplund, scourge of the Standard Solar Model.

Then, along comes Martin Asplund who carefully measures the abundance of elements in the Solar atmosphere with unprecedented care and detail, and he finds that some elements, in particular oxygen, have had their abundances overestimated by a lot.  This created, as the physicists like to say “tension” between the models and the data.

One solution to this problem is that the new abundances are wrong.  Another is that the Standard Solar Model has been wrong for decades, with offsetting errors that gave us a false sense of precision. The problem with this solution is: what’s the other offsetting error?

Steinn Sigurdsson pointed me to an intriguing possibility: maybe the Sun was more massive when it was young? This would have had many effects, including a larger buildup of helium in its core that would be inconsistent with helioseismic measurements.  But now that Asplund has “broken” helioseismology, maybe there’s some room to play here?

There’s not a lot of room to play with this: Brian Wood has been measuring mass loss in young stars and finds it’s too small to have much effect.  But those measurements are pretty uncertain, and the payoff here is big: the insolation of the planets goes as the fifth power (!) of the Sun’s mass (two powers from holding the planets closer and three from higher rates of fusion) so even a 1.01 solar mass young sun would have an important effect (5%) on their received flux when they were young.  In particular, a major problem in planetary science is the “Faint Young Sun paradox”: the young sun was 25% fainter than today, so how could early Mars and Earth have had liquid water?!  Perhaps this is part of the problem?

This is not a new idea; Sackmann and Boothroyd discussed it 13 years ago. But with the new Asplund abundances (and Bailey opacities) it’s time to revisit the problem.

Even if the young sun was faint, it was very active.  The repurposed Kepler mission K2 has been observing stars across a range of ages, seeing how their flare rates and energies vary with stellar age and mass. These are important inputs for models of the young Earth and Mars: high energy particles can have a big effect on young planets’ atmospheres.  Indeed, NExSS PI Vladimir Airapetian had a nice result on this recently with respect to the Faint Young Sun paradox.

Anthony Del Genio of the Goddard Institute for Space Studies

Anthony Del Genio of the Goddard Institute for Space Studies is interested in extending the GISS ROCKE-3D global climate model to early (Archaean) Earth, and the inputs for that model include the spectrum of the Sun at early times—a spectrum K2 will help us understand, and that depends on the mass of the Sun at that time.

Are you a recent heliophysics or astrophysics PhD that would like to help is with this problem?  Please consider applying to our NPP opportunity by July 1. The arrangement we have in mind is that you will work at Penn State with me primarily, co-advised by Tony (including trips to GISS to work on the climate modeling side).

If you are going to do this, please get in touch with us directly so that we can help you craft a competitive proposal to NASA.

I hope to see you at Penn State!

Evaporating Planets and Exoplanet Interiors with JWST

I’m pleased to announce three out-of-cycle opportunities to work with Penn State astronomers — including me! — through the NASA Nexus for Exoplanet System Science.  This cross-disciplinary research network is soliciting applications due July 1 for Nasa Postdoctoral Program fellows to come to Penn State to work on projects that cross disciplines and NExSS teams.  I’ll describe the two with me in these blog posts; the third is to work with Eric Ford on the statistical properties of exoplanets (read the ad!)

Below is the first opportunity.  I blogged about the second one here.

Evaporating Planets and Exoplanet Interiors with JWST.

We don’t really know what the interior of rocky planets are like. Even the Earth’s interior is mysterious: we can’t really go down and sample it, and there are big arguments about whether the samples we get from volcanoes are representative.  As a result, we don’t really know whether the mantle well-mixed, and we don’t know the water content of the Earth’s interior to an order of magnitude!

But these questions matter: the origin of Earth’s volatile budget and its plate tectonics are both highly uncertain and key components of the story of its habitability.  We need to know answers to these questions about exoplanets, but that seems pretty unlikely considering we can’t even agree on the answer for Earth, for which we will always have much more information than distant exoplanets.

Artist’s impression of a planet helpfully preparing a representative, backlit sample of its interior for study by astronomers.

Enter Kepler.

Among the new classes of exoplanets discovered by Kepler, KIC 12557548 represents the prototype of one that has particularly caught my eye: “evaporating” planets, a subset of “ultra-short period” planets (with periods less that 1 day).

These planets show highly asymmetric light curves, typically orbit M or K dwarfs, and are apparently rocky planets (or their leftover metallic cores) being ablated or evaporated by the intense instellation of their host star.  This process is, in some cases, stochastic, giving rise not just to asymmetric transits but extremely variable depths:

Transits of KIC 12557548 b, from Fig. 2 of Rappaport et al. 2012

KIC 12557548 is not alone.  At least three other similar planets have been detected, including K2-22 which is in many ways much easier to study.  Here, we have what appears to be representative samples of the interiors of exoplanet being spewed into space right where we can study them with spectrographs.

Can we do mineralogy of these materials? Can we study the hydration levels of the rock? Can we compute the volatile inventory of these planets’ mantles? Were these planets once habitable? Are these in fact the metallic cores of once-rocky planets, meaning that they likely once had magnetic fields?

Steve Desch introduces us to lots of exoplanets

I don’t know, but I’m dying to find out. Before he left for industry, PSU research associate Ming Zhao laid the groundwork for this study in coordination with Steve Desch’s NExSS group at ASU.  Steve’s group has been thinking hard about the infrared spectroscopic signatures of the minerals of these planets, and what they can tell us about the planet formation process, these planets’ past potential for habitability, and planet formation generally.

Neal Turner, another NExSS PI, has also been thinking about these effluents’ properties, their interaciton with their host star’s magnetic fields and winds, and, very importantly, how they might be affected by the intense instellation they receive.

Are you an emerging researcher in astrophysics or planetary science interested by this problem? Please consider applying to our NPP opportunity by July 1.  The arrangement we have in mind is that you will work at Penn State with me primarily, co-advised by Steve (including trips to ASU to work on the planetary science side) and Neal (ditto for JPL and the stellar effects side).

If you are going to do this, please get in touch with us directly so that we can help you craft a competitive proposal to NASA.

I hope to see you soon at Penn State!

It’s been a busy few weeks for studies of the fascinating star announced by Tabetha Boyajian’s team, KIC 8462852.

Kickstarter!

It’s official!  Tabetha Boyajian is leading a Kickstarter effort to fund long-term monitoring of KIC 8462852 (I’m on the team!).  The idea is to purchase time on LCOGT, a private network of small telescopes around the world.  These professional instruments can provide regular brightness measurements of bright stars like KIC 8462, and will be able to provide us with an alert if it starts doing one of its mysterious dimming events again.  It’s an important effort, and exactly the sort of expensive, unknown-probability, uncertain-payoff science that is very hard for conservative time allocation committees and grant proposal panels to approve.

The logo for Tabetha Boyajian’s Kickstarter campaign.

But it’s also the sort of fun and fascinating science that plenty of people would be willing to kick a few bucks towards, and if “plenty” times “few” turns out to be enough, we’ll be able to ensure that we don’t miss the next event.  Please go to the site and help us out!

An Atlantic Article

Ross Andersen from the Atlantic, who wrote the article that made Boyajian’s star famous, saw the recent back-and-forth by Schaefer and Hippke.  First, Schaefer showed that Boyajian’s star seems to have undergone a “century-long-fade.”  Hippke wrote a rebuttal, Schaefer wrote an acid response, and Hippke came back with a more careful rebuttal.

Kimberly M. S. Cartier a.k.a. @AstroKimCartier

Rather than write his own summary for The Atlantic, would I like to write it myself, he wondered?  As luck would have it, my PhD student Kimberly Cartier, who is starting her final year in graduate school, is pursuing a career in science journalism.  Would Ross be interested in a piece co-written by the two of us?  Sure, he said.

So Kim and I quickly whipped up a Google Doc and pounded out a story.  After some back-and-forth with Ross for style and content, it went up on The Atlantic’s website.  I think it came out really well!

You can find more of Kim’s science outreach and journalism at Universe Today’s weekly space hangout, at her blog, occasionally on Monday mornings at 98.7 the Freq, on on twitter at @AstroKimCartier.

Green Bank Time!

The Green Bank 100m telescope, the largest steerable telescope in the world.

The event that started Boyajian’s Star’s fame was when Ross Andersen met with Andrew Siemion in Washington after Andrew’s testimony to Congress about the search for life in the universe. At the time, Andrew, Tabby, and I had just recently submitted a proposal to NRAO to use the Green Bank 100 m telescope to “listen” to Boyajian’s Star for alien transmissions.  Ross wrote a nice article on the Congressional event based on an interview with Andrew.

That “fun talk”, included Andrew mentioning our Green Bank proposal, and the rest is history.

But whatever happened to the Green Bank proposal? Well, the TAC met before Ross’s story broke, so all they had to go on was our short proposal explaining why the star was weird.  Our proposal was not as compelling as Ross’s article, and they turned us down, “with prejudice” as the lawyers say.

NRAO has a scale for ranking proposals, prioritized ‘A’ through ‘C’ for proposals that are awarded time, to ‘N’ for those for which there’s just not enough time.  It turns out, there’s also a sub-basement on the scale: N*, meaning something like “rejected not for lack of time, but because the proposal is not worthy, even if time were available.”

N* is what we got.  We got the feedback shortly after the news broke, and we decided to try again the next semester.  With a lot of astronomers’ eyes on the star, we could argue that if there were a simple exaplanation, it would have been forthcoming by now.  We also got to mention the Schaefer/Hippke flap, and address some of the TAC comments from the first round.

Well, apparently it worked!  We were just awarded 25 hours of ‘C’ time for 2016B, and Andrew tells me that this means we will almost certainly be able to observe.  I’m looking forward to the trip to West Virginia with Tabby and Andrew to do some radio astronomy!

That’s all for now.  Stay tuned…

Lodén 1 Part IV: Clusters in the Era of Gaia

So last time we established that the putative middle-aged, nearby cluster Lodén1 is neither middle-aged, nor nearby, nor a cluster.

(That, by the way, was basically the title of our paper, but the referee really disliked it (they thought it was confusing to call it a cluster then say it isn’t a cluster). Then the copyeditor went and changed all of our “amongst”s to “among”s.  Ah, well.)

We still need to take a look at NGC 2240 just in case, but frankly it’s pretty obviously not a real cluster, so it’s a low priority.  Also, Gaia is coming, and it will make this whole endeavor much easier.

The rest of this post is some thoughts by Jason Curtis on the topic:

While Lodén 1 does not appear to be a real cluster, the existence and recent realization that Ruprecht 147 is the oldest nearby cluster suggests that similar clusters might have also gone overlooked. As we say in our paper, “the utility of such clusters for stellar astrophysics demands that we find them.” This fall, the European Space Agency will begin releasing high-precision position and velocity data produced by its Gaia mission, starting with the brightest 2 million stars that were observed by the Hipparcos satellite in the early 1990s.

This first catalog will reach stars like the Sun at distances of up to 1000 light years, including the majority of the proposed candidates of Lodén 1 and the membership of Ruprecht 147. We expect that the improved proper motion precision will enhance our ability to determine the nature of unproven clusters like Lodén 1 and improve the membership identification of established clusters like Ruprecht 147.

Artist’s impression of Gaia

The stars that make up a cluster travel together through the galaxy, with little spread in position (e.g., clusters can span 10—20 light years) and velocity (typically 500 m/s, whereas the cluster itself can travel at tens of km/s relative to neighboring stars). Within a few years, Gaia will release 3D positions (coordinates and parallaxes) and 3D space motions (proper motions and radial velocities) for some 150 million stars, while fainter stars will still receive 3D positions and 2D proper motions. Even sparse star clusters like Ruprecht 147 are 2—3 times denser than the Solar neighborhood. This is not a huge contrast; however, the inclusion of ultra-high-precision proper motions from Gaia (which will see a 100—200x increase in precision over existing proper motions) will make finding sparse clusters easy!

Gaia’s measurements will let us….

1. “Weigh” clusters by measuring velocity dispersion from proper motions
2. Resolve internal structure of nearby clusters with parallaxes, and eliminate distance uncertainty for others
3. Enable easy cluster identification by looking for over-densities in 5D phase space (3D positions—including parallax— and proper motions). Basically, stars are distributed throughout the Solar neighborhood and nearby galactic environment with a characteristic density or spacing. Clusters, even sparse clusters, should appear as over-densities given the expected high precision of the parallaxes. Furthermore, the stars in a given few parsec volume do not exhibit coherent proper motion. Together, these 5 position/motion components should yield new clusters, and new members of known clusters.

Lots to do, but first we should search for bound and moderately rich (N>20) systems that can immediately be characterized and targeted by space missions like TESS.

Our paper is now on the arXiv and will soon appear in the Astronomical Journal.

A Question for METI Critics

In a new paper (put putting forth an old argument) John Gertz argues that attempts to send deliberate signals for detection by alien civilizations is “unwise, unscientific, potentially catastrophic, and unethical.”  His rather caustic assault on METI-proponents is a pretty good summary of the extreme METI-opponent position. (METI = Messaging to ExtraTerrestrial Intelligences).

One thing that caught my eye that I had not heard before is that he obliquely proposes that something like an ethics review board weigh in on any powerful transmissions made by Earth.  He specifically mentions Arecibo radar pulses used to probe Solar System objects:

The asteroid detection radar problem is very easy to fix by adopting a standard of best practices that includes a provision for muting the radar during moments when the target occults a nearby star or transits the plane of the Milky Way.

The agent of our destruction?

I may be behind the times here, but this is the first time I’ve heard that the planetary science community should consider the ethical implications to the planet for their observations (as opposed to just the ethical implications of the deaths of any birds that happen to fly above the dish during transmission).

But Gertz interestingly does not mention laser AO programs, which send powerful laser beams to some of the nearest stars routinely.  Indeed, Kipping & Teachy recently showed how relatively powerful lasers from other worlds would be easily noticed as artificial signals even with our present technology, and searches for pulsed laser emission is one of the most promising SETI routes we have.  Tellis & Marcy have searched for lasers as weak as tens of Watts coming from tens of AU away from nearby stars.  I haven’t run the numbers, but it would surprise me if our laser AO systems, pointed right at nearby stars, were not detectable by an advanced alien civilization as being obviously artificial.

So my honest question to Gertz and other METI opponents is whether we should seriously be setting up review boards for laser AO and planetary radar?  What about the powerful arctic radars used to look for ICBMs that sweep across the sky? How powerful or coherent must a transmission be before we consider its ethical implications?

As a METI agnostic, I don’t have an answer to these questions; I’m genuinely curious to have this discussion.

Lodén 1, Part III: Neither Old, Nor Nearby, Nor a Cluster

Last time I described how the photometry of the stars in the purported cluster Lodén 1 didn’t seem to really implicate a cluster.

The next step was to get some radial velocities. Jason Curtis submitted a proposal to SALT—the South Africa Large Telescope—to use the Robert Stobie Spectrograph (RSS).  Lodén 1 is in the Southern Hemisphere, so we couldn’t use HET, but SALT is an HET clone, and in exchange for the plans and lessons learned on HET, the HET consortium, including Penn State, got institutional access to SALT for a few years.

The South Africa Large Telescope.

The telescope was still working out its growing pains, so we never got all of the observations we asked for, and the reduction pipeline improved as we went along, but in the end we got some nice spectra of two classes of stars: Lodén’s original candidates, and the members identified by Kharchenko.

Eunkyu Han, now a graduate student at Boston University.

The reduction and analysis was done by Eunkyu Han, at the time a post-baccalaureate researcher for our group, and now a graduate student in Phil Muirhead’s group at Boston University.  Eunkyu did a lot of work reducing all of the data from SALT down to just the number we wanted: the radial velocity  Thanks a lot to the SALT staff for helping us with the reductions and wavelength solutions on this relatively new and untested instrument!

These medium resolution spectra measure radial velocities to a km/s or so.  This is enough to see if they’re all roughly the same (in the case of a co-moving group of stars in a cluster) or basically random (as we’d expect for field stars).  This is what they look like:

Medium-resolution spectrum of Lodén’s candidate 5.

All of this light is roughly in the orange portion of the spectrum, with yellow off the left hand side and deep red off the right hand side. The deep lines marked “Na D” are where the star is dark, exactly at the color of those orange sodium street lamps. This is due to sodium in the star’s atmosphere. The inverse-Eiffel-Tower shape on the right is from hydrogen in the star’s atmosphere. The difference in the wavelengths of these lines as we observe them and as they are in the lab tells us how fast the star is moving towards or away from us. We actually used the narrow lines marked in red to make this determination. (The blue line shows at which wavelengths the Earth’s atmosphere messes with the measurements—you can see why we avoided those regions!).

So, is there a cluster of stars all at the same velocity, distinct from “the field”?  Or does it look basically like you’d expect for random stars?  Here’s Eunkyu’s result (in black) and what we expect from a random collection of stars in that direction (from Jason Curtis):

Radial velocity distribution of candidate Lodén 1 members. Nothing to see here; move along…

Yeah, there’s not much there.  There is a peak, but it’s about where you expect to find one, anyway.  We plotted up the stars in that peak and found… nothing that looks like a coeval sequence in the photometry.

So:

• We looked at the colors of the stars, and found lots of A stars, so its not old.
• We looked at a color magnitude diagram, and nothing stood out from the field, so if anything is there, it’s not bright, so it’s not nearby.
• And looking at the motions of the stars, it’s exactly what you expect from the field.

In short, the old, nearby cluster Lodén 1 is neither old, nor nearby, nor a cluster.

Paging Linda Richman…

So this one didn’t pan out, but, as we wrote in the paper, “The potential utility that would come with the discovery of a new 2 Gyr star cluster at a distance of only 360 pc was sufficiently high that it warranted careful inspection and disproof.”

We did get into a semantic argument with the referee about whether if there is any cluster or association in the field that Gaia might find, it would be Lodén 1 or not.  We decided not; your mileage may vary.

Next time: Final thoughts, and cluster hunting in the era of Gaia.