About

Annalee Baker, MD, is an Associate Professor of Emergency Medicine at Rutgers New Jersey Medical School. She completed her medical education at Penn State University and her residency training at NYU Langone/Bellevue Hospital Center. Her professional interests include medical education, mentorship, professional development, and advocacy, focusing on advancing emergency medicine through education and supporting the growth of medical professionals in her field.

Research topics

• Astronomy
• Astrophysics
• Physics

Selected publications

• V <i>z</i> -GAL: Probing Cold Molecular Gas in Dusty Star-forming Galaxies at <i>z</i> = 1–6

  The Astrophysical Journal Supplement Series · 2026-01-23

  articleOpen access

  Abstract We present the first results of V z -GAL, a high-redshift CO( J = 1–0) large survey with the Karl G. Jansky Very Large Array, targeting 92 Herschel-selected, infrared-luminous, dusty star-forming galaxies at redshifts 1–6. These sources are selected based on having redshifts and mid-/high- J CO transitions from the NOrthern Extended Millimeter Array z –GAL survey. We successfully detect CO( J = 1–0) emission in 90/92 galaxies at the expected positions and redshifts, including nine tentative detections at 2 σ –3 σ significance, and CO( J = 2–1) emission in 10 of these galaxies. The CO( J = 1–0) luminosities suggest apparent gas masses in the range <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>μ</mml:mi> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:msub> <mml:mrow> <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> </mml:msub> </mml:mrow> </mml:msub> </mml:math> = (2–20) × 10 11 ( α CO /4.0) M ⊙ , which implies gas depletion times of 50–600 Myr. These timescales show similar spread as local ULIRGs, suggesting a self-regulatory mechanism that maintains a consistent star formation rate per unit gas mass in starbursts across redshifts. To quantify the contribution of “excitation correction” factors to gas mass estimates, we calculate median CO line brightness temperature ratios of r 21 = 0.88 ± 0.25, r 31 = 0.61 ± 0.22, r 41 = 0.49 ± 0.15, r 51 = 0.47 ± 0.13, and r 61 = 0.28 ± 0.13. Accounting for these corrections results in a reduced scatter in “gas mass–star formation rate” relations. We also find a median log( <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>L</mml:mi> <mml:msub> <mml:mrow> <mml:mo accent="true">′</mml:mo> </mml:mrow> <mml:mrow> <mml:mo stretchy="false">[</mml:mo> <mml:mi mathvariant="normal">CI</mml:mi> <mml:mo stretchy="false">]</mml:mo> <mml:msup> <mml:mrow> <mml:mo stretchy="false">(</mml:mo> </mml:mrow> <mml:mrow> <mml:mn>3</mml:mn> </mml:mrow> </mml:msup> <mml:msub> <mml:mrow> <mml:mi>P</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>1</mml:mn> </mml:mrow> </mml:msub> <mml:msup> <mml:mrow> <mml:mo>−</mml:mo> </mml:mrow> <mml:mrow> <mml:mn>3</mml:mn> </mml:mrow> </mml:msup> <mml:msub> <mml:mrow> <mml:mi>P</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>0</mml:mn> </mml:mrow> </mml:msub> <mml:mo stretchy="false">)</mml:mo> </mml:mrow> </mml:msub> <mml:mo>/</mml:mo> <mml:mi>L</mml:mi> <mml:msub> <mml:mrow> <mml:mo accent="true">′</mml:mo> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">CO</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:mi>J</mml:mi> <mml:mo>=</mml:mo> <mml:mn>1</mml:mn> <mml:mo>−</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="false">)</mml:mo> </mml:mrow> </mml:msub> <mml:mo stretchy="false">)</mml:mo> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:mn>0.71</mml:mn> <mml:mo>±</mml:mo> <mml:mn>0.12</mml:mn> </mml:math> for a subsample of 23 sources, consistent with the ratios derived for local star-forming galaxies. Together, our findings are in agreement with common conditions in the cold gas reservoirs among star-forming galaxies over a broad range in star formation modes, efficiencies, and scales.

  PublisherDOI

• The RESOLVE and ECO G3 Initiative: Drivers of HI Content and X-ray Emission in Galaxy Groups

  ArXiv.org · 2025-04-17

  preprintOpen access

  Adding to the RESOLVE and ECO Gas in Galaxy Groups (G3) initiative, we examine possible drivers of group-integrated HI-to-halo mass ratios ($M_{\rm HI,grp}/M_{\rm halo}$) and group X-ray emission, including group halo mass ($M_{\rm halo}$), virialization as probed by crossing time ($t_{\rm cross}$), presence of active galactic nuclei (AGN), and group-integrated fractional stellar mass growth rate (FSMGR$_{\rm grp}$). G3 groups span $M_{\rm halo}=10^{11-14.5}\,M_\odot$ with comprehensive HI and AGN information, which we combine with X-ray stacking of ROSAT All-Sky data. We detect hot gas emission exceeding AGN and X-ray binary backgrounds confidently for $M_{\rm halo}=10^{12.6-14}\,M_\odot$ and unambiguously for $M_{\rm halo}&gt;10^{14}\,M_\odot$, reflecting an inverse dependence of $M_{\rm\,HI,grp}/M_{\rm halo}$ and hot gas emission on halo mass. At fixed halo mass, $M_{\rm\,HI,grp}/M_{\rm halo}$ transitions to greater spread below $t_{\rm cross}\sim2$ Gyr. Dividing groups across this transition, lower-$t_{\rm cross}$ groups show elevated X-ray emission compared to higher-$t_{\rm cross}$ groups for $M_{\rm halo}&gt;10^{13.3}\,M_\odot$, but this trend reverses for $M_{\rm halo}=10^{12.6-13.3}\,M_\odot$. Additionally, AGN-hosting halos below $M_{\rm halo}\sim10^{12.1}\,M_\odot$ exhibit a broad, $\sim$0.25 dex deep valley in $M_{\rm HI,grp}/M_{\rm halo}$ compared to non-AGN-hosting halos with correspondingly reduced FSMGR$_{\rm grp}$. When diluted by non-AGN-hosting halos, this valley becomes shallower and narrower, falling roughly between $M_{\rm halo}=10^{11.5}\,M_\odot$ and $M_{\rm halo}=10^{12.1}\,M_\odot$ in the overall $M_{\rm\,HI,grp}/M_{\rm\,halo}$ vs. $M_{\rm halo}$ relation. We may also detect a second, less easily interpreted valley at $M_{\rm halo}\sim10^{13}\,M_\odot$. Neither valley matches theoretical predictions of a deeper valley at or above $M_{\rm halo}=10^{12.1}\,M_\odot$.

  PublisherOA PDFDOI

• HerS-3: An Exceptional Einstein Cross Reveals a Massive Dark Matter Halo

  The Astrophysical Journal · 2025-09-16 · 1 citations

  articleOpen accessCorresponding

  Abstract We present a study of HerS-3, a dusty star-forming galaxy at z spec = 3.0607, which is gravitationally amplified into an Einstein cross with a fifth image of the background galaxy seen at the center of the cross. Detailed 1 mm spectroscopy and imaging with NOEMA and the Atacama Large Millimeter/submillimeter Array resolve the individual images and show that each of the five images display a series of molecular lines that have similar central velocities, unambiguously confirming that they have identical redshifts. The Hubble Space Telescope F110W image reveals a foreground lensing group of four galaxies with a photometric redshift z phot ∼ 1.0. Lens models that only include the four visible galaxies are unable to reproduce the properties of HerS-3. By adding a fifth massive component, lying southeast of the brightest galaxy of the group, the source reconstruction is able to match the peak emission, shape, and orientation for each of the five images. The fact that no galaxy is detected near that position indicates the presence of a massive dark matter halo in the lensing galaxy group. In the source plane, HerS-3 appears as an infrared luminous starburst galaxy seen nearly edge on. The serendipitous discovery of this exceptional Einstein cross offers a potential laboratory for exploring at small spatial scales a nuclear starburst at the peak of cosmic evolution and studying the properties of a massive dark matter halo associated with the lensing galaxy group.

  PublisherDOI

• Testing OH Megamaser Identification Methods in H <scp>i</scp> Surveys: Updated Source-flagging Algorithms and New Detections in ALFALFA

  The Astrophysical Journal · 2025-06-06

  articleOpen accessCorresponding

  Abstract OH megamasers (OHMs) are extragalactic masers found primarily in gas-rich galaxy major mergers. To date, only ∼120 OHMs have been cataloged since their discovery in 1982, and efforts to identify distinct characteristics of OHM host galaxies have remained inconclusive. As radio astronomy advances with next-generation telescopes and extensive 21 cm H i surveys, precursors to the Square Kilometre Array are expected to detect the 18 cm OH masing line with significantly increased frequency, potentially expanding the known OHM population tenfold. These detections, however, risk confusion with lower-redshift H i emitters unless accompanied by independent spectroscopic redshifts. Building on methods proposed by Roberts et al. for distinguishing these interloping OHMs via near- to mid-IR photometry and emission line frequencies, we apply these techniques to data from the Arecibo Legacy Fast ALFA [Arecibo L -band Feed Array] (ALFALFA) survey and a preliminary Aperture Tile In Focus (Apertif) H i emission line catalog from the Westerbork Synthesis Radio Telescope. Our study, utilizing the Apache Point Observatory 3.5 m telescope to obtain optical spectroscopic redshifts of 142 candidates (107 from ALFALFA and 35 from Apertif), confirms five new OHM host galaxies and reidentifies two previously catalogued OHMs misclassified as H i emitters in ALFALFA. These findings support the predictions from Roberts et al. and underscore the evolving landscape of radio astronomy in the context of next-generation telescopes.

  PublisherDOI

• The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H i–Halo Mass Relation

  UNC Libraries · 2025-06-12

  articleOpen access

  We present a four-step group-finding algorithm for the Gas in Galaxy Groups (G3) initiative, a spin-off of the z &sim; 0 REsolved Spectroscopy Of a Local VolumE (RESOLVE) and Environmental COntext (ECO) surveys. In preparation for future comparisons to intermediate redshift (e.g., the LADUMA survey), we design the group finder to adapt to incomplete, shallow, or nonuniform data. We use mock catalogs to optimize the group finder&rsquo;s performance. Compared to friends-of-friends (with false-pair splitting), the G3 algorithm offers improved completeness and halo-mass recovery with minimal loss of purity. Combining it with the volume-limited H i census data for RESOLVE and ECO, we examine the H i content of galaxy groups as a function of group halo mass. Group-integrated H i mass M H I,grp rises monotonically over halo masses M halo &sim; 1011&ndash;1014.5 M ⊙, pivoting in slope at M halo &sim; 1011.4 M ⊙, the gas-richness threshold scale. We present the first measurement of the scatter in this relation, which has a median of &sim;0.3 dex and is asymmetric toward lower M H I,grp. We discuss interesting tensions with theoretical predictions and prior measurements of the M H I,grp&ndash;M halo relation. In an appendix, we release RESOLVE DR4 and ECO DR3, including updates to survey redshifts, photometry, and group catalogs, as well as a major expansion of the ECO H i inventory with value-added data products.

  PublisherDOI

• Erratum: “The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H <scp>i</scp>–Halo Mass Relation” (2023, ApJ, 956, 51)

  The Astrophysical Journal · 2025-05-30

  erratumOpen accessCorresponding
  PublisherDOI

• Erratum: “The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H i–Halo Mass Relation” (2023, ApJ, 956, 51)

  UNC Libraries · 2025-06-12

  articleOpen access

  Erratum to &ldquo;The RESOLVE and ECO Gas in Galaxy Groups Initiative: The Group Finder and the Group H i&ndash;Halo Mass Relation&rdquo;

  PublisherDOI

• The RESOLVE and ECO G3 Initiative: Drivers of H <scp>i</scp> Content and X-Ray Emission in Galaxy Groups

  The Astrophysical Journal · 2025-05-27 · 1 citations

  articleOpen accessCorresponding

  Abstract Adding to the RESOLVE and ECO Gas in Galaxy Groups (G3) initiative, we examine possible drivers of group-integrated H i -to-halo mass ratios ( M HI,grp / M halo ) and group X-ray emission, including group halo mass ( M halo ), virialization as probed by crossing time ( t cross ), presence of active galactic nuclei (AGN), and group-integrated fractional stellar mass growth rate (FSMGR grp ). G3 groups span M halo = 10 11 −10 14.5 M ⊙ with comprehensive H i gas and AGN information, which we combine with X-ray stacking of ROSAT All-Sky data. We detect hot gas emission exceeding AGN and X-ray binary backgrounds confidently for M halo = 10 12.6 −10 14 M ⊙ and unambiguously for M halo &gt; 10 14 M ⊙ , reflecting an inverse dependence of M HI,grp / M halo and hot gas emission on halo mass. At fixed halo mass, M HI,grp / M halo transitions to greater spread below t cross ∼ 2 Gyr. Dividing groups across this transition, lower- t cross groups show elevated X-ray emission compared to higher- t cross groups for M halo &gt; 10 13.3 M ⊙ , but this trend reverses for M halo = 10 12.6 −10 13.3 M ⊙ . Additionally, AGN-hosting halos below M halo ∼ 10 12.1 M ⊙ exhibit a broad, ∼0.25 dex deep valley in M HI,grp / M halo compared to non-AGN-hosting halos with correspondingly reduced FSMGR grp . When diluted by non-AGN-hosting halos, this valley becomes shallower and narrower, falling roughly between <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mi>M</mml:mi> <mml:mrow> <mml:mi mathvariant="normal">halo</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:msup> <mml:mn>10</mml:mn> <mml:mrow> <mml:mn>11.5</mml:mn> </mml:mrow> </mml:msup> <mml:mspace width="0.25em"/> <mml:msub> <mml:mi>M</mml:mi> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> </mml:math> and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mi>M</mml:mi> <mml:mrow> <mml:mi mathvariant="normal">halo</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:msup> <mml:mn>10</mml:mn> <mml:mrow> <mml:mn>12.1</mml:mn> </mml:mrow> </mml:msup> <mml:mspace width="0.25em"/> <mml:msub> <mml:mi>M</mml:mi> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> </mml:math> in the overall M HI,grp / M halo vs. M halo relation. We may also detect a second, less easily interpreted valley at M halo ∼ 10 13 M ⊙ . Neither valley matches theoretical predictions of a deeper valley located at or above <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mi>M</mml:mi> <mml:mrow> <mml:mi mathvariant="normal">halo</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:msup> <mml:mn>10</mml:mn> <mml:mrow> <mml:mn>12.1</mml:mn> </mml:mrow> </mml:msup> <mml:mspace width="0.25em"/> <mml:msub> <mml:mi>M</mml:mi> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> </mml:math> .

  PublisherDOI

• Looking at the Distant Universe with the MeerKAT Array: The H <scp>i</scp> Mass Function in the Local Universe

  The Astrophysical Journal · 2025-03-10 · 2 citations

  articleOpen access

  Abstract We present measurements of the neutral atomic hydrogen (H i ) mass function (H i MF) and cosmic H i density (Ω H I ) at 0 ≤ z ≤ 0.088 from the Looking at the Distant Universe with MeerKAT Array (LADUMA) survey. Using LADUMA Data Release 1 (DR1), we analyze the H i MF via a new “recovery matrix” method that we benchmark against a more traditional modified maximum likelihood (MML) method. Our analysis, which implements a forward modeling approach, corrects for survey incompleteness and uses extensive synthetic source injections to ensure robust estimates of the H i MF parameters and their associated uncertainties. This new method tracks the recovery of sources in mass bins different from those in which they were injected and incorporates a Poisson likelihood in the forward modeling process, allowing it to correctly handle uncertainties in bins with few or no detections. The application of our analysis to a high-purity subsample of the LADUMA DR1 spectral line catalog in turn mitigates any possible biases that could result from the inconsistent treatment of synthetic and real sources. For the surveyed redshift range, the recovered Schechter function normalization, low-mass slope, and “knee” mass are <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>ϕ</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>*</mml:mo> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mn>3.5</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>6</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1.92</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.97</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo>×</mml:mo> <mml:mn>1</mml:mn> <mml:msup> <mml:mrow> <mml:mn>0</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>3</mml:mn> </mml:mrow> </mml:msup> </mml:math> Mpc −3 dex −1 , <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>α</mml:mi> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:mn>1.1</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>8</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.19</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.08</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> , and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>log</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>*</mml:mo> </mml:mrow> </mml:msub> <mml:mo>/</mml:mo> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> <mml:mo stretchy="false">)</mml:mo> <mml:mo>=</mml:mo> <mml:mn>10.0</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>1</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.12</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.31</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> , respectively, which together imply a comoving cosmic H i density of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mo mathvariant="normal">Ω</mml:mo> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">H</mml:mi> <mml:mspace width="0.25em"/> <mml:mi mathvariant="normal">I</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mn>3.0</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>9</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.47</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.65</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo>×</mml:mo> <mml:mn>1</mml:mn> <mml:msup> <mml:mrow> <mml:mn>0</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>4</mml:mn> </mml:mrow> </mml:msup> </mml:math> . Our results show consistency between recovery matrix and MML methods and with previous low-redshift studies, giving confidence that the cosmic volume probed by LADUMA, even at low redshifts, is not an outlier in terms of its H i content.

  PublisherDOI

• Modeling ALMA Observations of the Warped Molecular Gas Disk in the Red Nugget Relic Galaxy NGC 384

  The Astrophysical Journal · 2024-11-01 · 3 citations

  articleOpen access

  Abstract We present 0.″22 resolution CO(2–1) observations of the circumnuclear gas disk in the local compact galaxy NGC 384 with the Atacama Large Millimeter/submillimeter Array (ALMA). While the majority of the disk displays regular rotation with projected velocities rising to 370 km s −1 , the inner ∼0.″5 exhibits a kinematic twist. We develop warped disk gas-dynamical models to account for this twist, fit those models to the ALMA data cube, and find a stellar mass-to-light ratio in the H band of M / L H = 1.34 ± 0.01 [1 σ statistical] ±0.02 [systematic] M ⊙ / L ⊙ and a supermassive black hole (BH) mass ( M BH ) of M BH <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>=</mml:mo> <mml:mo stretchy="false">(</mml:mo> <mml:msubsup> <mml:mn>7.26</mml:mn> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.48</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.43</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo stretchy="false">[</mml:mo> <mml:mn>1</mml:mn> <mml:mi>σ</mml:mi> <mml:mspace width="0.25em"/> <mml:mi>statistical</mml:mi> <mml:msubsup> <mml:mo stretchy="false">]</mml:mo> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1.00</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.55</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo stretchy="false">[</mml:mo> <mml:mi>systematic</mml:mi> <mml:mo stretchy="false">]</mml:mo> <mml:mo stretchy="false">)</mml:mo> <mml:mo>×</mml:mo> <mml:msup> <mml:mn>10</mml:mn> <mml:mn>8</mml:mn> </mml:msup> <mml:mspace width="0.25em"/> <mml:msub> <mml:mi>M</mml:mi> <mml:mo>⊙</mml:mo> </mml:msub> </mml:math> . In contrast to most previous dynamical M BH measurements in local compact galaxies, which typically found over-massive BHs compared to the local BH mass−bulge luminosity and BH mass−bulge mass relations, NGC 384 lies within the scatter of those scaling relations. NGC 384 and other local compact galaxies are likely relics of z ∼ 2 red nuggets, and over-massive BHs in these relics indicate BH growth may conclude before the host galaxy stars have finished assembly. Our NGC 384 results may challenge this evolutionary picture, suggesting there may be increased scatter in the scaling relations than previously thought. However, this scatter could be inflated by systematic differences between stellar- and gas-dynamical measurement methods, motivating direct comparisons between the methods for NGC 384 and the other compact galaxies in the sample.

  PublisherDOI

Recent grants

• Collaborative Research: Observing the Cosmic Evolution of Neutral Hydrogen

  NSF · $337k · 2018–2024

• CAREER: The Cosmic Evolution of Dense Gas in Star-Forming Galaxies

  NSF · $736k · 2010–2019

• LADUMA: Reaching the Highest Redshifts with the Deepest HI Survey

  NSF · $392k · 2023–2026

• Nowhere Left to Hide: Closing in on Dusty Galaxies at High Redshift

  NSF · $292k · 2007–2012

Frequent coauthors

• D. J. Pisano

  396 shared

• M. D. Lehnert

  340 shared

• E. Schinnerer

  Max Planck Institute for Astronomy

  248 shared

• M. Vaccari

  Inter-university Institute for Data Intensive Astronomy

  243 shared

• John P. Hughes

  Khalifa University of Science and Technology

  239 shared

• M. J. Jarvis

  University of Oxford

  231 shared

• Kavilan Moodley

  226 shared

• Sheila J. Kannappan

  223 shared

Labs

• Emergency MedicinePI

Education

• M.D.

  University of Illinois at Chicago

• Other

  Rutgers New Jersey Medical School