<p>How do they know that this is a spherical shell of gas, and not just something like an Airy pattern-like artifact produced by the VLT's large interferometric aperture?</p>
<p>Image from: <a href="https://www.eso.org/public/images/eso0906b/" rel="nofollow noreferrer">https://www.eso.org/public/images/eso0906b/</a></p>
<p><a href="https://i.sstatic.net/oYu00.jpg" rel="nofollow noreferrer"><img src="https://i.sstatic.net/oYu00.jpg" alt="enter image description here" /></a></p>
<p>I get 180 pixels from center to the first minimum, and 72 pixels = 4 mas. That makes the first minimum at 10 mas or 4.8E-08 radians. The wavelengths are around 1.6 microns so that would correspond to a circular aperture of 40 meters using 1.22 λ/d.</p>
<p>Are they really sure this is a real shell, and not an Airy disk? How was that proven?</p>
<p>From <a href="https://www.eso.org/public/news/eso0906/" rel="nofollow noreferrer">https://www.eso.org/public/news/eso0906/</a></p>
<blockquote>
<p>“We were able to construct an amazing image, and reveal the onion-like structure of the atmosphere of a giant star at a late stage of its life for the first time,” says Antoine Mérand, member of the team. “Numerical models and indirect data have allowed us to imagine the appearance of the star before, but it is quite astounding that we can now see it, and in colour.”</p>
<p>Although it is only 15 by 15 pixel across, the reconstructed image shows an extreme close-up of a star 100 times larger than the Sun, a diameter corresponding roughly to the distance between the Earth and the Sun. This star is, in turn, surrounded by a sphere of molecular gas, which is about three times as large again.</p>
<p>T Leporis, in the constellation of Lepus (the Hare), is located 500 light-years away. It belongs to the family of Mira stars, well known to amateur astronomers. These are giant variable stars that have almost extinguished their nuclear fuel and are losing mass. They are nearing the end of their lives as stars, and will soon die, becoming white dwarfs. The Sun will become a Mira star in a few billion years, engulfing the Earth in the dust and gas expelled in its final throes.</p>
<p>Mira stars are among the biggest factories of molecules and dust in the Universe, and T Leporis is no exception. It pulsates with a period of 380 days and loses the equivalent of the Earth’s mass every year. Since the molecules and dust are formed in the layers of atmosphere surrounding the central star, astronomers would like to be able to see these layers. But this is no easy task, given that the stars themselves are so far away — despite their huge intrinsic size, their apparent radius on the sky can be just half a millionth that of the Sun.</p>
<p>“T Leporis looks so small from the Earth that only an interferometric facility, such as the VLTI at Paranal, can take an image of it. VLTI can resolve stars 15 times smaller than those resolved by the Hubble Space Telescope,” says Le Bouquin.</p>
<p>To create this image with the VLTI astronomers had to observe the star for several consecutive nights, using all the four movable 1.8-metre VLT Auxiliary Telescopes (ATs). The ATs were combined in different groups of three, and were also moved to different positions, creating more new interferometric configurations, so that astronomers could emulate a virtual telescope approximately 100 metres across and build up an image.</p>
<p>“Obtaining images like these was one of the main motivations for building the Very Large Telescope Interferometer. We have now truly entered the era of stellar imaging,” says Mérand.</p>
<p>A perfect illustration of this is another VLTI image showing the double star system Theta1 Orionis C in the Orion Nebula Trapezium. This image, which was the first ever constructed from VLTI data, separates clearly the two young, massive stars from this system. The observations themselves have a spatial resolution of about 2 milli-arcseconds. From these, and several other observations, the team of astronomers, led by Stefan Kraus and Gerd Weigelt from the Max-Planck Institute in Bonn, could derive the properties of the orbit of this binary system, including the total mass of the two stars (47 solar masses) and their distance from us (1350 light-years).</p>
</blockquote>

CC BY-SA 4.0
2018-12-04T16:06:59.687Z
You really should give qualified scientists a little credit. (If this were slashdot, you'd be raked over the coals!). They are fully cognizant of the diffraction limit(s) of their observational tools, not to mention how to compensate for such problems. BTW, did you even read the part of your quote about the long effective baseline they were using? That answers your question quite directly.
Carl Witthoft
CC BY-SA 4.0
2018-12-04T16:09:54.463Z
Note that the range of effective diameters included almost 100 m, so your 40 m estimate doesn't agree with the interferometric apertures. Also, as one of the figures in the paper shows, the effective beam of the combined data is a) significantly smaller than the stellar image; and b) elliptical, not circular.
Peter Erwin
CC BY-SA 4.0
2018-12-04T16:25:22.333Z
Figure 4 in Le Bouquin et al. (2009) [https://www.aanda.org/articles/aa/pdf/2009/10/aa11579-08.pdf] is the figure I was alluding to in my comment.
Peter Erwin
CC BY-SA 4.0
2018-12-04T18:32:50.770Z
@CarlWitthoft I don't disagree with you, but this is not really a proper answer, and is more of a comment, IMO.
StephenG - Help Ukraine
CC BY-SA 4.0
2018-12-04T18:55:04.750Z
@PeterErwin Thanks, that's a start! Those beam shapes in the bottom-right corners of each frame of Fig. 4  just show some threshold value of the main lobe, perhaps half-power or something similar (it's not stated) and my question is about what happens well outside that. Presumably in a longer publication there will be a more complete discussion of the shape of the effective beam at the position of the very weak ring. Note I'm not trying to forward that this is an Airy disk, and have only mentioned the apparent similarity to one, approximate agreement in scale, and asking of it being ruled out
uhoh
CC BY-SA 4.0
2018-12-04T19:01:19.933Z
@CarlWitthoft Scientific results are challenged all the time, that's the nature of how science works! Exciting results are shared in a timely way, and sometimes they are withdrawn or modified after further study. The faster-than-light neutrinos in Italy, several peaks of high statistical probability at the LHC, cold fusion, EM drive come to mind without even looking for a list. Careful questioning of spectacular results is perfectly reasonable. I've asked *How was that ruled out?*
uhoh
CC BY-SA 4.0
2018-12-04T19:04:19.143Z
"If this were slashdot, you'd be raked over the coals!" Luckily this is Stack Exchange; answers need to be answers to the question as asked, and comments need to be helpful. Presuming that I'm not a qualified scientist as well hurts my feelings, I'm crushed. ;-)
uhoh
CC BY-SA 4.0
2018-12-04T20:14:35.853Z
@uhoh -- I think part of the answer is that interferometric point-spread functions generally do *not* look like the PSF of single-aperture telescopes, with a circular, symmetric Airy disk. So even if the authors somehow unaccountably forgot to complete the interferometric reduction process, you wouldn't end up with a symmetric Airy disk anyway.
Peter Erwin
CC BY-SA 4.0
2018-12-04T23:46:59.617Z
@PeterErwin Yep. Here's an example of a [sampled aperture](https://astronomy.stackexchange.com/a/24182/7982) within a single telescope. It's straightforward to calculate the PSF there with a few (dozen) lines of script. But here the image is built up over several nights from several different sets of three "holes" rather than interfere them all at once, (they move the telescopes around in between) and I don't know know how they synthesize that to get one image.
uhoh
CC BY-SA 4.0
2021-02-04T00:28:01.383Z
@PeterErwin I've just asked [What does a “point spread function” look like for long exposures from the VLT's large interferometric aperture?](https://astronomy.stackexchange.com/q/41213/7982)
uhoh
<optics><angular-resolution><interferometry>
Are they really sure this isn't an Airy disk? How was that ruled out?
uhoh
# Are they really sure this isn't an Airy disk? How was that ruled out?

(Asked by: username_0 on 2018-12-04)

How do they know that this is a spherical shell of gas, and not just something like an Airy pattern-like artifact produced by the VLT's large interferometric aperture?

Image from: <https://www.eso.org/public/images/eso0906b/>

[![enter image description here](https://i.sstatic.net/oYu00.jpg)](https://i.sstatic.net/oYu00.jpg)

I get 180 pixels from center to the first minimum, and 72 pixels = 4 mas. That makes the first minimum at 10 mas or 4.8E-08 radians. The wavelengths are around 1.6 microns so that would correspond to a circular aperture of 40 meters using 1.22 λ/d.

Are they really sure this is a real shell, and not an Airy disk? How was that proven?

From <https://www.eso.org/public/news/eso0906/>

> “We were able to construct an amazing image, and reveal the onion-like structure of the atmosphere of a giant star at a late stage of its life for the first time,” says Antoine Mérand, member of the team. “Numerical models and indirect data have allowed us to imagine the appearance of the star before, but it is quite astounding that we can now see it, and in colour.”
>
> Although it is only 15 by 15 pixel across, the reconstructed image shows an extreme close-up of a star 100 times larger than the Sun, a diameter corresponding roughly to the distance between the Earth and the Sun. This star is, in turn, surrounded by a sphere of molecular gas, which is about three times as large again.
>
> T Leporis, in the constellation of Lepus (the Hare), is located 500 light-years away. It belongs to the family of Mira stars, well known to amateur astronomers. These are giant variable stars that have almost extinguished their nuclear fuel and are losing mass. They are nearing the end of their lives as stars, and will soon die, becoming white dwarfs. The Sun will become a Mira star in a few billion years, engulfing the Earth in the dust and gas expelled in its final throes.
>
> Mira stars are among the biggest factories of molecules and dust in the Universe, and T Leporis is no exception. It pulsates with a period of 380 days and loses the equivalent of the Earth’s mass every year. Since the molecules and dust are formed in the layers of atmosphere surrounding the central star, astronomers would like to be able to see these layers. But this is no easy task, given that the stars themselves are so far away — despite their huge intrinsic size, their apparent radius on the sky can be just half a millionth that of the Sun.
>
> “T Leporis looks so small from the Earth that only an interferometric facility, such as the VLTI at Paranal, can take an image of it. VLTI can resolve stars 15 times smaller than those resolved by the Hubble Space Telescope,” says Le Bouquin.
>
> To create this image with the VLTI astronomers had to observe the star for several consecutive nights, using all the four movable 1.8-metre VLT Auxiliary Telescopes (ATs). The ATs were combined in different groups of three, and were also moved to different positions, creating more new interferometric configurations, so that astronomers could emulate a virtual telescope approximately 100 metres across and build up an image.
>
> “Obtaining images like these was one of the main motivations for building the Very Large Telescope Interferometer. We have now truly entered the era of stellar imaging,” says Mérand.
>
> A perfect illustration of this is another VLTI image showing the double star system Theta1 Orionis C in the Orion Nebula Trapezium. This image, which was the first ever constructed from VLTI data, separates clearly the two young, massive stars from this system. The observations themselves have a spatial resolution of about 2 milli-arcseconds. From these, and several other observations, the team of astronomers, led by Stefan Kraus and Gerd Weigelt from the Max-Planck Institute in Bonn, could derive the properties of the orbit of this binary system, including the total mass of the two stars (47 solar masses) and their distance from us (1350 light-years).

**Tags:** optics, angular-resolution, interferometry
> **Comments:**
> **username_1**: You really should give qualified scientists a little credit. (If this were slashdot, you'd be raked over the coals!). They are fully cognizant of the diffraction limit(s) of their observational tools, not to mention how to compensate for such problems. BTW, did you even read the part of your quote about the long effective baseline they were using? That answers your question quite directly.  
> **username_2**: Note that the range of effective diameters included almost 100 m, so your 40 m estimate doesn't agree with the interferometric apertures. Also, as one of the figures in the paper shows, the effective beam of the combined data is a) significantly smaller than the stellar image; and b) elliptical, not circular.  
> **username_2**: Figure 4 in Le Bouquin et al. (2009) [https://www.aanda.org/articles/aa/pdf/2009/10/aa11579-08.pdf] is the figure I was alluding to in my comment.  
> **username_3**: @CarlWitthoft I don't disagree with you, but this is not really a proper answer, and is more of a comment, IMO.  
> **username_0**: @PeterErwin Thanks, that's a start! Those beam shapes in the bottom-right corners of each frame of Fig. 4  just show some threshold value of the main lobe, perhaps half-power or something similar (it's not stated) and my question is about what happens well outside that. Presumably in a longer publication there will be a more complete discussion of the shape of the effective beam at the position of the very weak ring. Note I'm not trying to forward that this is an Airy disk, and have only mentioned the apparent similarity to one, approximate agreement in scale, and asking of it being ruled out  
> **username_0**: @CarlWitthoft Scientific results are challenged all the time, that's the nature of how science works! Exciting results are shared in a timely way, and sometimes they are withdrawn or modified after further study. The faster-than-light neutrinos in Italy, several peaks of high statistical probability at the LHC, cold fusion, EM drive come to mind without even looking for a list. Careful questioning of spectacular results is perfectly reasonable. I've asked *How was that ruled out?*  
> **username_0**: "If this were slashdot, you'd be raked over the coals!" Luckily this is Stack Exchange; answers need to be answers to the question as asked, and comments need to be helpful. Presuming that I'm not a qualified scientist as well hurts my feelings, I'm crushed. ;-)  
> **username_2**: @uhoh -- I think part of the answer is that interferometric point-spread functions generally do *not* look like the PSF of single-aperture telescopes, with a circular, symmetric Airy disk. So even if the authors somehow unaccountably forgot to complete the interferometric reduction process, you wouldn't end up with a symmetric Airy disk anyway.  
> **username_0**: @PeterErwin Yep. Here's an example of a [sampled aperture](https://astronomy.stackexchange.com/a/24182/7982) within a single telescope. It's straightforward to calculate the PSF there with a few (dozen) lines of script. But here the image is built up over several nights from several different sets of three "holes" rather than interfere them all at once, (they move the telescopes around in between) and I don't know know how they synthesize that to get one image.  
> **username_0**: @PeterErwin I've just asked [What does a “point spread function” look like for long exposures from the VLT's large interferometric aperture?](https://astronomy.stackexchange.com/q/41213/7982)  

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