Seaborn: V0.5.0 (November 2014)

Waskom, Michael; Meyer, Kyle; Hobson, Paul; Halchenko, Yaroslav; Koskinen, Miikka; Miles, Alistair; Wehner, Daniel; Botvinnik, Olga; Megies, Tobias; cynddl,; Ziegler, Erik; Yarkoni, Tal; Zaytsev, Yury V.; Coelho, Luís Pedro; Cole, John B.; Augspurger, Tom; diego,; Hoppe, Travis; Seabold, Skipper; Cloud, Phillip; Hoyer, Stephan; Qalieh, Adel; Allan, Dan

doi:10.5281/zenodo.12710

Cited by 81 publications

(28 citation statements)

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“…This research made use of (Birrer et al 2015;Birrer & Amara 2018), (https://github.com/ ajshajib/dolphin), (Barkana 1999), (Oliphant 2015), (Jones et al 2001), (Astropy Collaboration 2013, (Kluyver et al 2016), (Hunter 2007), (Waskom et al 2014), (Bertin & Arnouts 1996), (Foreman-Mackey et al 2013), (Diemer 2018), (Schreiber 2018), and C -(https://github.com/Samreay/ChainConsumer).…”

Section: Appendix A: Mass and Light Alignmentsmentioning

confidence: 99%

Dark matter haloes of massive elliptical galaxies at z ∼ 0.2 are well described by the Navarro–Frenk–White profile

Shajib

Treu

Birrer

et al. 2021

Monthly Notices of the Royal Astronomical Society

108

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We investigate the internal structure of elliptical galaxies at z ∼ 0.2 from a joint lensing–dynamics analysis. We model Hubble Space Telescope images of a sample of 23 galaxy–galaxy lenses selected from the Sloan Lens ACS (SLACS) survey. Whereas the original SLACS analysis estimated the logarithmic slopes by combining the kinematics with the imaging data, we estimate the logarithmic slopes only from the imaging data. We find that the distribution of the lensing-only logarithmic slopes has a median 2.08 ± 0.03 and intrinsic scatter 0.13 ± 0.02, consistent with the original SLACS analysis. We combine the lensing constraints with the stellar kinematics and weak lensing measurements, and constrain the amount of adiabatic contraction in the dark matter (DM) halos. We find that the DM halos are well described by a standard Navarro–Frenk–White halo with no contraction on average for both of a constant stellar mass-to-light ratio (M/L) model and a stellar M/L gradient model. For the M/L gradient model, we find that most galaxies are consistent with no M/L gradient. Comparison of our inferred stellar masses with those obtained from the stellar population synthesis method supports a heavy initial mass function (IMF) such as the Salpeter IMF. We discuss our results in the context of previous observations and simulations, and argue that our result is consistent with a scenario in which active galactic nuclei feedback counteracts the baryonic-cooling-driven contraction in the DM halos.

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Section: Appendix A: Mass and Light Alignmentsmentioning

confidence: 99%

Dark matter haloes of massive elliptical galaxies at z ∼ 0.2 are well described by the Navarro–Frenk–White profile

Shajib

Treu

Birrer

et al. 2021

Monthly Notices of the Royal Astronomical Society

108

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show abstract

“…Simulations in this paper made use of the REBOUND code which can be downloaded freely at http://github.com/hannorein/rebound. This research also made use of the numpy (Oliphant 2006), matplotlib (Hunter 2007), and seaborn (Waskom et al 2014) Python packages.…”

Section: Acknowledgementsmentioning

confidence: 99%

Hidden Planets: Implications from ’Oumuamua and DSHARP

Rice

Laughlin

2019

ApJ

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The discovery of 'Oumuamua (1I/2017 U1), the first interstellar interloper, suggests an abundance of free-floating small bodies whose ejection into galactic space cannot be explained by the current population of confirmed exoplanets. Shortly after 'Oumuamua's discovery, observational results from the DSHARP survey illustrated the near-ubiquity of ring/gap substructures within protoplanetary disks, strongly suggesting the existence of a vast population of as-yet undetected wide-separation planets that are capable of efficiently ejecting debris from their environments. These planets have a 5 au and masses of order Neptune's or larger, and they may accompany ∼50% of newly formed stars (Zhang et al. 2018). We combine the DSHARP results with statistical constraints from current timedomain surveys to quantify the population of detectable icy planetesimals ejected by disk-embedded giant planets through gravity assists. Assessment of the expected statistical distribution of interstellar objects is critical to accurately plan for and interpret future detections. We show that the number density of interstellar objects implied by 'Oumuamua is consistent with 'Oumuamua itself having originated as an icy planetesimal ejected from a DSHARP-type system via gravity assists, with the caveat that 'Oumuamua's lack of observed outgassing remains in strong tension with a cometary origin. Under this interpretation, 'Oumuamua's detection points towards a large number of long-period giant planets in extrasolar systems, supporting the hypothesis that the observed gaps in protoplanetary disks are carved by planets. In the case that 'Oumuamua is an ejected cometary planetesimal, we conclude that LSST should detect up to a few interstellar objects per year of 'Oumuamua's size or larger and over 100 yr −1 for objects with r > 1 m.

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“…In the next decade, the combination of sensitivity and exquisite resolution of the Next Generation Very Large Array (ngVLA) may make studies at this high resolution possible for galaxies out to the Virgo cluster and beyond. (Barrett et al 2005), NumPy (Harris et al 2020), pandas (McKinney 2010, photutils (Bradley et al 2018), SciPy (Jones et al 2001-), seaborn (Waskom et al 2014) . Radial profiles of the input parameters to the modeling for the dust continuum (green dashed), hot gas (gold dash-dotted), outflowing cold gas (blue solid), and the ambient cold gas (light blue dotted) as described in Section 3.2.…”

Section: Discussionmentioning

confidence: 99%

Outflows from Super Star Clusters in the Central Starburst of NGC253

Levy,

Bolatto,

Leroy

et al. 2020

Preprint

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Young massive clusters play an important role in the evolution of their host galaxies, and feedback from the high-mass stars in these clusters can have profound effects on the surrounding interstellar medium. The nuclear starburst in the nearby galaxy NGC 253 at a distance of 3.5 Mpc is a key laboratory in which to study star formation in an extreme environment. Previous high resolution (1.9 pc) dust continuum observations from ALMA discovered 14 compact, massive super star clusters (SSCs) still in formation. We present here ALMA data at 350 GHz with 28 milliarcsecond (0.5 pc) resolution. We detect blueshifted absorption and redshifted emission (P-Cygni profiles) towards three of these SSCs in multiple lines, including CS 7−6 and H 13 CN 4−3, which represents direct evidence for previously unobserved outflows. The mass contained in these outflows is a significant fraction of the cluster gas masses, which suggests we are witnessing a short but important phase. Further evidence of this is the finding of a molecular shell around the only SSC visible at near-IR wavelengths. We model the P-Cygni line profiles to constrain the outflow geometry, finding that the outflows must be nearly spherical. Through a comparison of the outflow properties with predictions from simulations, we find that none of the available mechanisms completely explains the observations, although dust-reprocessed radiation pressure and O star stellar winds are the most likely candidates. The observed outflows will have a very substantial effect on the clusters' evolution and star formation efficiency.

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Seaborn: V0.5.0 (November 2014)

Cited by 81 publications

References 0 publications

Dark matter haloes of massive elliptical galaxies at z ∼ 0.2 are well described by the Navarro–Frenk–White profile

Dark matter haloes of massive elliptical galaxies at z ∼ 0.2 are well described by the Navarro–Frenk–White profile

Hidden Planets: Implications from ’Oumuamua and DSHARP

Outflows from Super Star Clusters in the Central Starburst of NGC253

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