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<!doctype html>
<html lang="en">
<head>
<meta charset="utf-8">
<title>Ringberg 2021: Virial Equilibrium</title>
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<!-- Slides! -->
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<div class="slides">
<section data-id="9e1f37193271406fc72e974be0a8a3fe">
<div class="sl-block" data-block-type="text" style="width: auto; height: auto;" data-block-id="fa1e26dfdc2f3050895879d1fc1c4f1a">
<div class="sl-block-content" data-placeholder-tag="h1" data-placeholder-text="Title Text" style="z-index: 11;">
<h1 style="font-size:200%; word-break: keep-all; hyphens: none;">Ringberg ISM 2021</h1>
<p> Cluster formation and fragmentation (CMF, IMF)
... or maybe more scattered questions about HMYSOs</p>
<br>
<p class="footer">Adam Ginsburg</p>
<p class="smaller3 footer">Assistant Professor<br>Department of Astronomy<br>University of Florida, Gainesville</p>
<!--<div class=smaller3>
John Bally, Ashley Barnes, Nate Bastian, Cara Battersby,
Henrik Beuther, Crystal Brogan, Yanett Contreras, Joanna
Corby, Jeremy Darling, Chris De Pree, Roberto Galván-Madrid,
Guido Garay, Jonathan Henshaw, Todd Hunter, J. M. Diederik
Kruijssen, Steven Longmore, Xing Lu, Fanyi Meng, Elisabeth A.C.
Mills, Juergen Ott, Jaime E. Pineda, Álvaro Sánchez-Monge,
Peter Schilke, Anika Schmiedeke, Daniel Walker, David Wilner,
Leonardo Testi, Rowan Smith, Ke Wang, James Dale, Robert
Loughnane, Erik Rosolowsky, Eric Koch, Ciriaco
Goddi, Brett McGuire, Dick Plambeck, Melvyn
Wright</div>-->
<div class=smaller2>
<ul>
<li> Postdoc: Allison Towner
<li> PhD: Desmond Jeff, Theo Richardson, Alyssa Bulatek, Nazar Budaiev
<li> REU: Justin Otter, Danielle Bovie, Josh Machado, Sydney Petz
<li> Undergrad: Madeline Hall, Michael Fero, Derod Deal, Parker Ormonde, Aden Dawson, Helen Radomski, Brice Tingle, Oketa Basha, Morgan Himes
</ul>
</div>
<div class=smaller2> Slides available at <a
href="https://keflavich.github.io/talks/RingbergISM2021.html">https://keflavich.github.io/talks/RingbergISM2021.html</a>
</div>
</div>
</div>
</section>
<section>
<h4> Questions about HMYSOs & clusters: </h4>
<ul>
<li class=fragment> How dense are forming clusters? (stellar density) </li>
<ul class=fragment>
<li> Dense enough to form high-mass stars by collisions? </li>
<li> Possible approach: ALMA-LB observations </li>
</ul>
<li class=fragment> How massive are YSOs? </li>
<ul class=fragment>
<li> Luminosity, dust-mass estimates are really bad </li>
<li> Possible approach: Dynamical mass measurements. Salt disks? Masers? </li>
</ul>
<li class=fragment> Do HMYSOs get their mass through disks? </li>
<ul class=fragment>
<li> We see disks, but mostly they have little mass compared to the stars </li>
<li> Competitive accretion? Inertial inflow? Collisions? </li>
</ul>
</ul>
</section>
<section>
<section>
<h4 style=""> How dense are cluster-forming regions? </h4>
<div>
<div style="float:left; width:90%">
<img src="orion_assets/otter_gemini_b3_overlay.png" style="max-width:100%">
</div>
</div>
</section>
<section>
<h4 style=""> OMC1 is denser than the ONC </h4>
<div>
<div style="float:left; width:90%">
<img src="orion_assets/otter_orion_density_map_npix64_5neighbor_3panel.png" style="max-width:100%">
</div>
<div> N<sup>*</sup><sub>OMC</sub>(Otter+ 2021) = 1.6 x 10<sup>5</sup> pc<sup>-3</sup> </div>
<div> N<sup>*</sup><sub>ONC</sub>(Otter+ 2021) = 0.6 x 10<sup>5</sup> pc<sup>-3</sup> </div>
<div> N<sup>*</sup><sub>ONC</sub>(Hillenbrand+ 1998) = 0.2 x 10<sup>5</sup> pc<sup>-3</sup> </div>
</div>
</section>
<section>
<h4 style=""> Many new disks in the OMC </h4>
<div>
<div style="float:left; width:60%">
<img src="colloquium_assets/OrionZoom.png" style="max-width:100%">
</div>
<div style="float:right; width: 20%;" class=smaller>
<img src="FrontiersAssets/JustinOtter.jpg" style='max-height:20%' align='right'>
Otter+, resubmitted
<br>
<hr>
FOV: 0.07 pc (16000 AU)
<br> 72 YSOs
<br> One "hot core"
</div>
</div>
<aside class=notes>
<ul>
<li> Lots of stars & outflows in a small environment
<li> Still no massive (OB) stars
</ul>
</aside>
</section>
<section>
<h4 style=""> Disk Gallery </h4>
<div>
<div style="float:left; width:90%">
<img src="orion_assets/otter_orion_b7_page3.png" style="max-width:100%">
</div>
</div>
</section>
</section>
<section>
<section>
<h4 style="z-index:25; position: relative; color: white; top:0%; left: 0%; text-align:center;"> Salts in Orion </h4>
<span class=image style="background-image:url(assets_orion/nrao19cb1_AI_V3_SD.png); margin-top:-10%; margin-left:-20%; height:150%; width:150%">
<div style="position: relative; top:56%; left:-20%; display: inline-block;">
<div style="background-color:rgba(105,105,105,0.3); text-align:left;" class="smaller2"><a style="color:rgb(20,200,255)" href="http://adsabs.harvard.edu/abs/2018ApJ...860..119G">Ginsburg+ 2018c</a></div>
<div style="background-color:rgba(105,105,105,0.3); text-align:left;" class="smaller2"><a style="color:rgb(20,200,255)" href="http://adsabs.harvard.edu/abs/2019arXiv190104489G">Ginsburg+ 2019b</a></div>
<div style="background-color:rgba(105,105,105,0.3); text-align:left;" class="smaller2"><a style="color:rgb(20,200,255)" href="https://public.nrao.edu/news/2019-alma-salt-star/">Press Release on "ALMA salt star"</a></div>
</div>
</span>
<aside class=notes>
<ul>
<li> Artists conception of a disk around a high-mass protostar
<li> There is an outflow
<li> Note the blue hazy inner ring
</ul>
</aside>
</section>
<section>
<span class=image style="background-image:url(assets_orion/Trapezium_GEMS_mosaic_redblueorange_normed_small_contrast_bright_fullsize.png); margin-top:-2%; height:100%; position: absolute;">
</span>
<span class="fragment image" style="background-image:url(assets_orion/gems_saltdisk_composite_fullsize.png); margin-top:-2%; height:100%; position: absolute;">
<h4 style="position: absolute; color: white; top:0%; left: 30%;"> Orion Source I<br>
<div class=fragment>a disk around a 15 M<sub>⊙</sub> YSO </div>
</h4>
<div class=fragment style="position: relative; left:-17%; top:28%; color:white;" class=smaller>Salt: NaCl</div>
</span>
<div style="position: relative; bottom: -90%; left:20%" class="smaller3"><a class=darkbg href="https://www.gemini.edu/node/12343">Image: Ginsburg, NRAO</a></div>
<aside class=notes>
<ul>
<li> Orion Source I lives at the center of the BN/KL explosion
<li> We observed the disk known as source I
<li> ...in salts! NaCl and KCl
<li> We used that disk to measure the mass of the central source
</ul>
</aside>
</section>
<section>
<div><img style="float:left; width:60%" src="orion_assets/tanaka_salts.png" ></div>
<div><img style="width:40%" src="assets_orion/NaCl_G17.png"></div>
<div>
Left: Tanaka+ 2020, pair of NaCl-bearing disks.
<br>
Right: G17, Maud+ 2020
<div>
</section>
<section>
<span class=image style="background-image:url(assets_orion/NaCl_rotational_diagrams.png); height:100%">
<h2 style='text-align: left'> Temperature? </h2>
</span>
</section>
<section>
<span class=image style="background-image:url(assets_orion/KCl_rotational_diagrams.png); height:100%">
<h2 style='text-align: left'> Temperature? </h2>
</span>
</section>
<section>
<span class=image style="background-image:url(assets_orion/simulated_populations_with_wacky_radiation_field.svg); height:100%">
<h2 style='text-align: right; background-color:white; width:50%; position: relative; left:50%;'> A contrived model </h2>
</span>
</section>
<section>
<h4> Observing the Keplerian rotation profile of a disk is the most direct way to measure a protostar's mass </h4>
<div class=smaller2>(we can only see the disk, not the star itself)</div>
<span class=image style="background-image:url(assets_orion/Unknown_4_pp_pv_plots_fittedmodel_15msun_comparepv.png); margin-top:0%; height:78%">
<aside class=notes>
<ul>
<li> Left is a model position-velocity diagram, right is the data
<li> Red curve traces the outermost position of orbits of point particles
</ul>
</aside>
</section>
</section>
<section>
<section id=e2ezoomin>
<h4> W51 e2e: Too optically thick at 1mm to measure disk</h4>
<span class="image" style="background-image: url(colloquium_assets/W51e2_cycle3green_SiO_outflows_aplpy_zoom.png); height:85%;">
<div style="position: relative; top:92%; left:-23%;" class="smaller2"><a class=darkbg href="http://adsabs.harvard.edu/abs/2018arXiv180505364G">Goddi+ 2020</a></div>
</span>
<aside class=notes>
<ul>
<li> No emission lines from a disk were detected
<li> Continuum appears to be high optical depth in inner ~few hundred AU
</ul>
</aside>
</section>
<section>
<h4> CS v=0 J=1-0 and v=0 J=2-1 masers trace the disk? </h4>
<img src="colloquium_assets/W51e2e_sio_outflow_with_CS_contours.png" style='max-height:95%'>
<div style="position: relative; top:-90%; left:25%;" class="smaller2"><a class=darkbg href="http://adsabs.harvard.edu/abs/2019AJ....158..208G">Ginsburg+ 2019</a></div>
<aside class=notes>
<ul>
<li> If CS traces a disk (which requires assuming very, very hard),
the implied mass is ~24 Msun, which is reasonable.
</ul>
</aside>
</section>
<section>
<div>
<div style="float:left; width:50%">
<img src="colloquium_assets/vanderwaltfig10.png">
</div>
<div style="float:left; width:50%">
<h4> CS maser conditions</h4>
<a href="https://ui.adsabs.harvard.edu/#abs/2020arXiv201110420V/abstract">van der Walt+ 2020</a>
<ul class=smaller>
<li> Top: CS J=1-0, Bottom: CS J=2-1 </li>
<li> <span style="color:red">Red:</span> Consistent w/W51e2e observations </li>
<li> Masers do not coexist; require different specific CS column <br>(N<sub>2-1</sub>=10<sup>15.6</sup>, N<sub>1-0</sub>10<sup>16.1</sup> cm<sup>-2</sup>)</li>
<li> Require high abundance (X<sub class=smaller>CS</sub> > 10<sup class=smaller2>-5</sup>) </li>
<li> Hot (300-500 K), moderate-density (n~10<sup>5</sup> cm<sup>-3</sup>): Disk surface? Or outflow cavity wall?
</ul>
</div>
</div>
</section>
<section>
<h3> We can use salts to measure HMYSO masses </h3>
<ul>
<li class=fragment> NaCl, KCl are only in the disk, not the outflow <div class=smaller>(water traces both)</div>
<li class=fragment> NaCl is detected in at least two other HMYSOs
<div class=smaller>
(<a href="https://ui.adsabs.harvard.edu/abs/2020ApJ...900L...2T/abstract">Tanaka+ 2020</a>,
Maud+ in prep)</div>
<li class=fragment> Salts are observable with ALMA, the JVLA, and the future ngVLA
<li class=fragment> Future projects will involve observing and modeling salt disks to measure HMYSO masses
</ul>
</section>
</section>
<section>
<section>
<h4> Zooming in: W51-IRS2 </h4>
<img src="almaimf-w51-assets/W51_IRS2_almaimf_parent.png" style='max-height:80%'>
</section>
<section>
<h4> Zooming in: W51-IRS2 </h4>
<img src="almaimf-w51-assets/W51_IRS2_almaimf_lb_zoom.png" style='max-height:80%'>
</section>
<section>
<h4> Zooming in: W51-IRS2 </h4>
<img src="almaimf-w51-assets/W51_IRS2_almaimf_lb_rezoom.png" style='max-height:80%'>
</section>
<section>
<div style="float: left; max-width:70%; max-height:70%">
<img src="colloquium_assets/goddi2020_outfloww51irs2.png">
</div>
<div style='float: left; width:30%;'>
<span class="smaller" align=right style="position: relative; float: right;">
Goddi+ 2020: The outflow (& disk) around W51 North changed direction by ~50 deg
in < 100 years.
</span>
</div>
</section>
</section>
<section>
<h4> Questions about HMYSOs & clusters: </h4>
<ul>
<li > How dense are forming clusters? (stellar density) </li>
<ul >
<li> Dense enough to form high-mass stars by collisions? </li>
<li> Possible approach: ALMA-LB observations </li>
</ul>
<li > How massive are YSOs? </li>
<ul >
<li> Luminosity, dust-mass estimates are really bad </li>
<li> Possible approach: Dynamical mass measurements. Salt disks? Masers? </li>
</ul>
<li > Do HMYSOs get their mass through disks? </li>
<ul >
<li> We see disks, but mostly they have little mass compared to the stars </li>
<li> Competitive accretion? Inertial inflow? Collisions? </li>
</ul>
</ul>
</section>
</div>
</div>
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