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Extending the simulations of intermediate-mass black hole mass measurements to Virgo Cluster using ELT/HARMONI high resolution integral-field stellar kinematics

T0 review · 2 major / 8 minor · reviewed 2026-08-05 · deepseek-v4-flash

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Pith's one-line read Simulations indicate ELT/HARMONI can detect 2.5e5 solar-mass black holes in Virgo dwarfs.

desk verdict A believable closed-loop recovery, but the detectability claim rests on an untested central cusp slope; deserves refereeing with conditions. read the letter →

arxiv 2509.03364 v1 pith:TYCJ2K3T submitted 2025-09-03 astro-ph.GA

Hai N Ngo , Dieu D. Nguyen , Truong N. Nguyen , Trung H. Dang , Tien H.T. Ho This is my paper · ORCID
classification astro-ph.GA
keywords intermediate-massblackholesnuclearstarclustersELT/HARMONIstellarkinematicsJeansAnisotropicModelingVirgoClustermockintegral-fieldspectroscopyholemassmeasurement
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

Intermediate-mass black holes are the likely seeds of supermassive black holes, but almost none are confirmed beyond the Local Group because their gravitational spheres of influence are too small for current telescopes. This paper tries to establish that the forthcoming ELT/HARMONI can change that at Virgo Cluster distances of 16.5 Mpc. Using VCC 1861, a faint dwarf elliptical with a nuclear star cluster, the authors build a realistic mass model from HST imaging, generate mock HARMONI observations with and without a 2.5e5 solar-mass central black hole, and ask whether the black-hole mass can be recovered from the simulated stellar kinematics. They find that the high-resolution H-high and K-long gratings at 10 mas spaxels produce a clear central peak in velocity dispersion when the IMBH is present and a central drop when it is not, and that Bayesian recovery returns the input mass to within about 0.05-0.09 dex. If this holds, ELT/HARMONI will be able to measure IMBHs in Virgo dwarfs and begin mapping their occupation fraction, directly testing seeding scenarios for supermassive black holes.

What carries the argument

The load-bearing observable is the inner velocity-dispersion profile: within the central roughly 0.1 arcsec, the black hole's gravity creates a sigma peak, whereas a cluster without a black hole shows a sigma drop. Whether that contrast survives depends on the central stellar density, which the authors extrapolate from 0.11 arcsec HST photometry to the 0.01 arcsec HARMONI pixel scale using a core-Sersic profile with a fixed inner power-law index gamma=0.1. The simulation chain then links a Multi-Gaussian Expansion mass model, JAMcyl anisotropic Jeans models, HSIM mock-cube generation, pPXF spectral fitting, and adaptive-Metropolis MCMC to recover masses. The main degeneracy is an anti-correl

What would settle it

Re-running the same mock pipeline on VCC 1861 with a different inner power-law index (for example gamma=0.5 instead of 0.1) would test whether the central velocity-dispersion peak of the 2.5e5 solar-mass IMBH remains distinguishable from the no-black-hole case; if the profiles become indistinguishable, the central claim fails. Equivalently, a real 4.5-hour ELT/HARMONI observation of VCC 1861 showing no central sigma peak would contradict the predicted detectability.

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Extended reading notes

Core claim

The paper reports that ELT/HARMONI's high-resolution H-high and K-long gratings at 10 mas spaxels can detect and measure a 2.5e5 solar-mass IMBH in the nuclear star cluster of VCC 1861 at 16.5 Mpc. The simulated black hole creates a central velocity-dispersion peak of about 24 km/s inside 0.1 arcsec, while the no-black-hole model produces a central drop, so the two cases are clearly distinguishable. Bayesian Jeans Anisotropic Modeling recovers log(M_BH/Msun)=5.382±0.049 in H-high and 5.337±0.090 in K-long against an input of 5.4, with the mass-to-light ratio near the input value of 1.4. The no-black-hole cubes yield upper limits of 3.18 and 2.54 in log(M_BH/Msun), so the same pipeline can bo

Load-bearing premise

The central stellar density profile is extrapolated from 0.11 arcsec Hubble resolution down to 0.01 arcsec ELT pixels using a core-Sersic model with a fixed inner slope gamma=0.1, and if the real nuclear cusp is steeper or shallower the claimed 5% detectability could disappear.

Editorial extensions

If this is right

  • ELT/HARMONI high-resolution gratings at 10 mas spaxels can distinguish a 2.5e5 solar-mass IMBH from a no-black-hole nuclear star cluster at 16.5 Mpc.
  • In the no-black-hole case the method returns tight upper limits, so it can also rule out IMBHs at the 5% mass contrast.
  • The H-high and K-long gratings yield consistent kinematics with differences below 5%, giving an internal cross-check on the recovered masses.
  • The recovered black-hole mass is accurate to about 0.05-0.09 dex, and the mass-to-light ratio is recovered near its input value.
  • This extends IMBH searches from the Local Group out to Virgo Cluster distance, substantially enlarging the volume over which IMBH demographics can be probed.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The same pipeline could be pointed at other Virgo dwarf galaxies with nuclear star clusters; a survey of detections and non-detections would measure the IMBH occupation fraction in dwarfs, which the paper does not attempt.
  • The fixed gamma=0.1 inner slope is the least tested input; if ELT resolves the true nuclear cusp, comparing the assumed and observed profiles would directly test the detectability calculation.
  • Because the field of view covers only the nuclear star cluster, inclination is poorly constrained; adding the galaxy's outer disk in future simulations could reduce the mass-to-light versus black-hole-mass degeneracy and tighten the recovery.
  • A central sigma-peak-versus-drop dichotomy, if generic, would make cheap IMBH screening possible from short observations before expensive full MCMC modeling.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 8 minor

Summary. The paper presents a simulation study assessing whether ELT/HARMONI high-resolution integral-field stellar kinematics can measure intermediate-mass black holes (IMBHs) in Virgo Cluster dwarf galaxies. The authors build a stellar mass model of VCC 1861 from HST/ACS imaging, extrapolated to sub-HST scales with a core-Sersic profile (γ=0.1), construct noiseless mock cubes using JAMcyl, pass them through the HSIM instrument simulator for the H-high and K-long high-resolution gratings with LTAO, extract kinematics with Voronoi binning and pPXF, and recover the BH mass via JAMcyl+MCMC. For an injected IMBH of log M_BH=5.4, they recover 5.38 (H-high) and 5.34 (K-long); for the no-BH case they place upper limits. They conclude that ELT/HARMONI can detect IMBHs with masses about 5% of the host nuclear star cluster mass at 16.5 Mpc.

Significance. If the central claim holds, the paper provides a valuable feasibility forecast: extending IMBH dynamical mass measurements from the Local Volume (≲3.5 Mpc) to the Virgo Cluster distance would dramatically increase the sample of accessible IMBH candidates. The study uses a realistic instrument simulation pipeline (HSIM, LTAO, Voronoi binning, pPXF with a 13-template library) and the recovery of the injected BH mass is clean. However, the test is a closed-loop exercise—the same JAMcyl model family, the same MGE, and the same template library are used for both mock generation and fitting—and the central stellar density profile is extrapolated below HST resolution using a fixed, untested core-Sersic slope. These two issues make the headline detectability claim conditional on unvalidated structural assumptions. The paper also offers a concrete, falsifiable prediction about HARMONI's capabilities, which is useful for planning ELT observations.

major comments (2)
  1. [Section 3.1] The central MGE component has σ=0.008″ (Table 1), about 10 times smaller than the HST/ACS PSF FWHM (0.11″). It is derived from a core-Sersic fit with γ=0.1 fixed 'as assumed by [41]' and extrapolated below the HST resolution to the 10 mas spaxel scale. This component sets the stellar density inside the BH sphere of influence (R_soi≈17 mas) and directly controls the contrast between the BH and no-BH Vrms profiles that underlies the detectability claim in Sections 4.1 and 4.2. The authors acknowledge the need to 'extrapolate deeply toward the center' but do not test alternative γ values. If the actual NSC cusp is steeper (e.g., γ=0.5 or 1.0), the central stellar mass would be larger and could mimic or mask a 2.5×10^5 M⊙ BH, changing the 5% detectability threshold. Please add sensitivity tests with at least two alternative inner slopes (or a non-parametric MGE) and quantify the effect on th
  2. [Sections 3.2 and 4.2] The mock data are generated with JAMcyl using the same MGE, β_z=0.02, M/L=1.4, and the same MARCS library that are used in the pPXF extraction and the JAMcyl fit. The recovery of log M_BH=5.38/5.34 is therefore primarily a check of internal consistency of the MCMC and the instrument pipeline. The claim of 'the ELT's capability to detect IMBHs' overstates the evidence: real galaxies have unknown anisotropy, possible M/L gradients, and unmeasured central density slopes. Please either (i) run a robustness test with mock data generated at different β_z and with a different MGE inner slope, verifying that the recovery remains unbiased, or (ii) soften the abstract and conclusion to state that the detectability is conditional on the assumed stellar mass profile. As written, this is a load-bearing caveat for the central claim.
minor comments (8)
  1. [Section 1] Affiliation contains the typo 'Physisc' for 'Physics'.
  2. [Section 3.1] The PSF is described as 'HST/WFPC2 F850LP'; the observations are ACS/WFC, so this should be corrected.
  3. [Section 3.2] Text says 'pixel size of 5 × 5 mas2. This pixel size is smaller than the 10 × 10 arcsec² of ELT/HARMONI'—the units should be '10 × 10 mas²'.
  4. [Section 4.2] The text refers to inclination spanning '300 − 900' and a 'best fit at 300'; these should be '30°–90°' and '30°' (or, given the input of 44° stated in Section 3.2, the statement 'aligning with our input parameters' is incorrect).
  5. [Section 4.2] The chi-squared equation is mangled: '∑ (V_rms,i − V̅_rms,i)^n' should be 'Σ (V_rms,i − V̅_rms,i)^2 / σ^2', and the meaning of σ in that expression should be clarified.
  6. [Figure 5 caption] The caption says 'medium resolution gratings,' but the paper uses the H-high and K-long high-resolution gratings; this appears to be a copy-paste error.
  7. [Table 2] The 'Input Parameters' column lists prior ranges, not the true input values. Please add a separate column (or row) with the injected values (i=44°, M/L=1.4, log M_BH=5.4) so the recovery can be directly compared.
  8. [Section 4.1] The statement 'β_z is also well-constrained with the difference of Δβ_z < 0.1' is not supported by Table 2: the no-BH K-long row reports β_z = 0.007 ± 0.240. This claim should be qualified or removed.

Circularity Check

2 steps flagged · score 5.0 of 10

Detectability claim is contingent on an assumed central cusp (gamma=0.1) imported from the authors' own prior simulation and on a closed-loop JAMcyl recovery; instrument simulation adds independent content.

  1. ansatz smuggled in via citation [Section 3.1 (Galaxy mass model)]
    "Notably, our chosen ELT/HARMONI pixel size of 0.01" (spatial resolution), which is five times smaller than the given HST observation. We need to extrapolate deeply toward the center. To do that, we fit the surface brightness profile with the core-Sersic [57], [58] and Sersic [59] function using non-linear least-squares method via MPFIT package [60]. As assumed by [41], the stellar mass distribution in NSC can be described using core-Sersic with the power law index of γ = 0.1."

    The central power-law index γ=0.1 is not measured from HST data; the MGE's central Gaussian has σ=0.008 arcsec, far smaller than the 0.11 arcsec HST PSF, so the central profile is an extrapolation. The assumption is imported from [41], a prior simulation paper by the same group (D. D. Nguyen et al. 2024). This assumed cusp sets the central stellar density, which directly controls the contrast between the MBH=2.5e5 Msun and no-BH kinematics in Section 4.1. The paper tests no alternative slopes, so the ELT detectability claim is conditional on an ansatz taken from the authors' own prior work rather than on an independent constraint.

  2. other [Section 3.2 (Mock HSIM IFS cube creating) and Section 4.2 (Bayesian inference)]
    "We created two noiseless cubes: MBH = 0 and 𝑀BH = 2.5 × 10^5 𝑀⊙ using mass model from Section 3.1. ... The Vrms profile derived from pPXF fitting is used for BH mass recovery. We apply a Bayesian inference framework to derive the best-fitting JAMcyl parameters..."

    The 'mass model from Section 3.1' is a fixed MGE, and it is also the stellar mass model used in the JAMcyl fit. The mock cubes are generated by JAMcyl with an injected MBH, and the fit recovers MBH with JAMcyl using the same fixed stellar mass distribution. Thus the recovered MBH is the input MBH by construction (up to noise); this is a closed-loop consistency check, not an independent measurement or prediction. The instrument simulation (HSIM) and pPXF extraction are genuine external steps, but the astrophysical signal contrast is predetermined by the same model used in the fit, so the central detectability claim partly restates the simulation inputs.

full rationale

The paper is a simulation study, so some degree of closed-loop recovery is methodologically standard. However, the central claim that ELT/HARMONI can detect an IMBH of 5% of the NSC mass at Virgo distance rests on two steps that are partly circular. First, the central stellar cusp slope is assumed γ=0.1 by citation to [41], a prior simulation by the same authors, and this assumption controls the BH-vs-no-BH contrast; no alternative slopes are tested. Second, the mock data are generated and fitted with the same JAMcyl model family and the same fixed MGE, so the successful mass recovery is largely a consistency check. The HSIM instrument simulation, pPXF kinematics extraction, and realistic noise are independent elements that do provide real content, preventing a higher score. The verdict is partial circularity: the capability forecast is conditional on the imported ansatz and the closed-loop model, not fully independent.

Assumptions & free parameters 4 free parameters · 4 assumptions · 0 invented entities

The central feasibility claim rests on a small number of adopted parameters (M/L, beta_z, gamma, inclination) and on the assumption that the same JAMcyl model that generates the mock data can recover them. No new physical entities are introduced.

free parameters (4)
  • Constant mass-to-light ratio M/L_F850LP = 1.4 (M_sun/L_sun)
    Adopted from empirical (g-z) color relation [61] to convert HST F850LP luminosity to stellar mass; directly sets the stellar mass in the JAM model. A different M/L changes the inferred BH mass.
  • Anisotropy parameter beta_z = 0.02
    Assumed constant, from the VIRUS-dE survey [67]. Sets the shape of the LOSVD; a different value changes the Vrms profile and the BH mass recovery.
  • Core-Sersic power-law index gamma = 0.1
    Assumed for the NSC component following [41]. Controls the central stellar density profile after extrapolation to ELT scales.
  • Inclination i = 44 degrees
    Assumed when generating the mock cubes; not constrained by the data (posterior spans 30-90 degrees). Affects the projected kinematics.
assumptions (4)
  • domain assumption The NSC mass distribution follows the MGE model derived from HST surface brightness with a constant M/L.
    Used in Section 3.1 to construct the mass model; the stellar density profile anchors all kinematic predictions.
  • domain assumption JAMcyl with axisymmetric velocity ellipsoid, cylindrical alignment, and constant anisotropy beta_z is an adequate dynamical model.
    Invoked in Section 3.2; the mock data are generated and recovered with the same model family.
  • ad hoc to paper The core-Sersic profile can be safely extrapolated below the HST resolution to 0.01 arcsec.
    Section 3.1; the paper acknowledges this extrapolation ('We need to extrapolate deeply toward the center') but does not test alternative central slopes.
  • domain assumption The stellar population is described by MARCS SPS spectra at 5 Gyr, solar metallicity, and a Salpeter IMF.
    Used in Sections 3.2 and 4.1; template mismatch could bias kinematic extraction, though 13 templates are used in pPXF.

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Cite this review

Pith. "Pith review of Extending the simulations of intermediate-mass black hole mass measurements to Virgo Cluster using ELT/HARMONI high resolution integral-field stellar kinematics." pith.science (2026). https://pith.science/paper/TYCJ2K3T

@misc{pith2026250903364,
  author       = {Pith},
  title        = {Pith review of: Extending the simulations of intermediate-mass black hole mass measurements to Virgo Cluster using ELT/HARMONI high resolution integral-field stellar kinematics},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/TYCJ2K3T}},
  note         = {Machine review of arXiv:2509.03364}
}
abstract

The firm co-existence of intermediate-mass black holes (IMBHs, $M_{\rm BH} \approx 10^3-10^6 M_odot$) in nuclear star clusters (NSCs) remains uncertain because the limited number of verified instances within the local Universe, limited within 3.5 Mpc. They are crucial for our understanding about the formation and evolution of supermassive black holes (SMBHs). The upcoming Extremely Large Telescope (ELT) promises to revolutionize the detection of these mysterious objects. In this study, we simulated the kinematics of an IMBH within the nuclear star cluster of VCC 1861, one of the faintest galaxies in the Virgo Cluster. Using Jeans Anisotropic Modeling (JAM) and stellar density profiles derived from Hubble Space Telescope (HST) data and the HSIM program, we created mock High Angular Resolution Monolithic Optical and Near-infrared Integral field spectrograph (HARMONI) observations for the ELT. We then extract stellar kinematics from these mock data and recover the BH mass using the JAM model with Markov Chain Monte Carlo simulation method. Our results demonstrate the ELT's capability to detect IMBHs with masses comprising 5% of the NSC's mass at the distance of the Virgo Cluster.

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Reference graph

Works this paper leans on

80 extracted references · 18 canonical work pages

  1. [41]

    Improved Dynamical Constraints on the Masses of the Central Black Holes in Nearby Low-mass Early-type Galactic Nuclei and the First Black Hole Determination for NGC 205,

    D. D. Nguyen et al., “Improved Dynamical Constraints on the Masses of the Central Black Holes in Nearby Low-mass Early-type Galactic Nuclei and the First Black Hole Determination for NGC 205,” Astrophys. J., vol. 872, no. 1, p. 104, Feb. 2019, doi: 10.3847/1538-4357/aafe7a

    doi:10.3847/1538-4357/aafe7a 2019

  2. [1]

    Currently, we knew that the stellar mass black holes (BHs, 𝑀𝐵𝐻 ≲ 102𝑀⊙) is massive star remnants [1]

    Introduction The intermediate-mass black holes ( IMBHs, with a mass range of 102 ≲ 𝑀𝐵𝐻 ≲ 106𝑀⊙) existence in below-Milky Way mass galaxies (𝑀⋆ ≲ 5 × 1010𝑀⊙) is important to our knowledge of the origins of SMBHs (SMBHs, 𝑀𝐵𝐻 ≳ 106𝑀⊙) in early Universe. Currently, we knew that the stellar mass black holes (BHs, 𝑀𝐵𝐻 ≲ 102𝑀⊙) is massive star remnants [1]. In c...

    work page

  3. [2]

    It hosts numerous dwarf galaxies which predicted to harbor IMBHs [43], [44]

    Simulated Virgo cluster target: VCC 1861 Virgo Cluster is the one of the largest galaxy clusters at North hemisphere with  2,000 members [42]. It hosts numerous dwarf galaxies which predicted to harbor IMBHs [43], [44] . With its diversity in galaxy demographics [45], it provides perfect targets for studying galaxy evolution. VCC 1861 (or IC 3652) is a t...

    work page

  4. [3]

    We generated the mock IFS data cube s with the HARMONI Simulation (HSIM a) program [52]

    Methodology In this section, we simulated mock observations using the HARMONI instrument of the ELT. We generated the mock IFS data cube s with the HARMONI Simulation (HSIM a) program [52]. To achieve this, we first built a galaxy mass model based on Hubble Space Telescope ( HST) images (Section 3.1). We then constructed a noiseless IFS cubes using this m...

    work page

  5. [4]

    Finally, we summarized these findings in Section 5

    work page

  6. [5]

    Kinematic extracting Firstly, we used the V oronoi binning method to merge adjacent pixels and achieve a signal-to-noise ratio 𝑆/𝑁 ≳ 20 for each bin using the vorbin package [73]

    Result 4.1. Kinematic extracting Firstly, we used the V oronoi binning method to merge adjacent pixels and achieve a signal-to-noise ratio 𝑆/𝑁 ≳ 20 for each bin using the vorbin package [73]. Next, we fitted the spectra of these bins to the MARCS spectral library using the Penalized Pi Xel-Fitting (pPXF) method [74]. The LOSVD was fitted using the Gauss-H...

    work page

  7. [6]

    In this upcoming future , ELT promises to improve the detection of these objects

    Conclusion These IMBHs are crucial to knowledge of the formation mechanism and evolution of SMBHs. In this upcoming future , ELT promises to improve the detection of these objects. In this study, we have focused on the ability of ELT in IMBH detecting with galaxies in Virgo Cluster (distance of 𝐷 ≈ 16.5 Mpc). This aims to expand the survey further than th...

    work page 2022

  8. [7]

    On Continued Gravitational Contraction,

    J. ~R. Oppenheimer and H. Snyder, “On Continued Gravitational Contraction,” Phys. Rev., vol. 56, no. 5, pp. 455–459, Sep. 1939, doi: 10.1103/PhysRev.56.455

    doi:10.1103/physrev.56.455 1939

Show all 80 references
  1. [8]

    Iron Emission in the z = 6.4 Quasar SDSS J114816.64+525150.3,

    A. J. Barth, P. Martini, C. H. Nelson, and L. C. Ho, “Iron Emission in the z = 6.4 Quasar SDSS J114816.64+525150.3,” Astrophys. J., vol. 594, no. 2, p. L95, Aug. 2003, doi: 10.1086/378735

    2003 doi

  2. [9]

    A luminous quasar at a redshift of z = 7.085,

    D. J. Mortlock et al., “A luminous quasar at a redshift of z = 7.085,” Nature, vol. 474, no. 7353, pp. 616–619, Jun. 2011, doi: 10.1038/nature10159

    2011 doi

  3. [10]

    Izumi et al., “Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs)

    T. Izumi et al., “Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XIII. Large-scale Feedback and Star Formation in a Low-luminosity Quasar at z = 7.07 on the Local Black Hole to Host Mass Relation,” Astrophys. J., vol. 914, no. 1, p. 36, Jun. 2021, doi: 10.3847/...

    2021 doi

  4. [11]

    EIGER. III. JWST/NIRCam Observations of the Ultraluminous High-redshift Quasar J0100+2802,

    A.-C. Eilers et al., “EIGER. III. JWST/NIRCam Observations of the Ultraluminous High-redshift Quasar J0100+2802,” Astrophys. J., vol. 950, no. 1, p. 68, Jun. 2023, doi: 10.3847/1538-4357/acd776

    2023 doi

  5. [12]

    ALMA confirmation of an obscured hyperluminous radio-loud AGN at z = 6.853 associated with a dusty starburst in the 1.5 deg2 COSMOS field,

    R. Endsley et al., “ALMA confirmation of an obscured hyperluminous radio-loud AGN at z = 6.853 associated with a dusty starburst in the 1.5 deg2 COSMOS field,” Mon. Not. R. Astron. Soc., vol. 520, no. 3, pp. 4609–4620, 2023, doi: 10.1093/mnras/stad266

    2023 doi

  6. [13]

    A small and vigorous black hole in the early Universe,

    R. Maiolino et al., “A small and vigorous black hole in the early Universe,” Nature, pp. 1–3, 2024

    2024

  7. [14]

    Massive black holes lurking in Milky Way satellites,

    S. van Wassenhove, M. Volonteri, M. ~G. Walker, and J. ~R. Gair, “Massive black holes lurking in Milky Way satellites,” Monthly Notices of the Royal Astronomical Society, vol. 408, no. 2, pp. 1139–1146, Oct. 2010, doi: 10.1111/j.1365- 2966.2010.17189.x

    2010

  8. [15]

    The Formation and Evolution of Massive Black Holes,

    M. Volonteri, “The Formation and Evolution of Massive Black Holes,” Science (80-. )., vol. 337, no. 6094, p. 544, Aug. 2012, doi: 10.1126/science.1220843

    2012 doi

  9. [16]

    An Upper Limit to the Velocity Dispersion of Relaxed Stellar Systems without Massive Black Holes,

    M. C. Miller and M. B. Davies, “An Upper Limit to the Velocity Dispersion of Relaxed Stellar Systems without Massive Black Holes,” Astrophys. J., vol. 755, no. 1, p. 81, Aug. 2012, doi: 10.1088/0004-637X/755/1/81

    2012 doi

  10. [17]

    MOCCA code for star cluster simulations - IV. A new scenario for intermediate mass black hole formation in globular clusters,

    M. Giersz, N. Leigh, A. Hypki, N. Lützgendorf, and A. Askar, “MOCCA code for star cluster simulations - IV. A new scenario for intermediate mass black hole formation in globular clusters,” Monthly Notices of the Royal Astronomical Society, vol. 454, no. 3, pp. 3150–3165, Dec. ...

    2015 doi

  11. [18]

    The fate of dense stellar systems,

    M. C. Begelman and M. J. Rees, “The fate of dense stellar systems,” Mon. Not. R. Astron. Soc., vol. 185, no. 4, pp. 847–860, 1978, doi: 10.1093/mnras/185.4.847

    1978 doi

  12. [19]

    A SAURON study of M32: measuring the intrinsic flattening and the central black hole mass,

    E. ~K. Verolme et al., “A SAURON study of M32: measuring the intrinsic flattening and the central black hole mass,” Monthly Notices of the Royal Astronomical Society, vol. 335, no. 3, pp. 517–525, Sep. 2002, doi: 10.1046/j.1365-8711.2002.05664.x

    2002

  13. [20]

    Low-mass black holes as the remnants of primordial black hole formation,

    J. E. Greene, “Low-mass black holes as the remnants of primordial black hole formation,” Nat. Commun., vol. 3, p. 1304, Dec. 2012, doi: 10.1038/ncomms2314

    2012 doi

  14. [21]

    Massive black hole seeds born via direct gas collapse in galaxy mergers: their properties, statistics and environment,

    S. Bonoli, L. Mayer, and S. Callegari, “Massive black hole seeds born via direct gas collapse in galaxy mergers: their properties, statistics and environment,” Monthly Notices of the Royal Astronomical Society, vol. 437, no. 2, pp. 1576–1592, Jan. 2014, doi: 10.1093/mnras/stt1990

    2014 doi

  15. [22]

    An actively accreting massive black hole in the dwarf starburst galaxy Henize 2-10,

    A. E. Reines, G. R. Sivakoff, K. E. Johnson, and C. L. Brogan, “An actively accreting massive black hole in the dwarf starburst galaxy Henize 2-10,” Nature, vol. 470, no. 7332, pp. 66–68, 2011, doi: 10.1038/nature09724

    2011 doi

  16. [23]

    A POPULATION OF INTERMEDIATE-MASS BLACK HOLES IN DWARF STARBURST GALAXIES UP TO REDSHIFT = 1.5,

    M. Mezcua, F. Civano, G. Fabbiano, T. Miyaji, and S. Marchesi, “A POPULATION OF INTERMEDIATE-MASS BLACK HOLES IN DWARF STARBURST GALAXIES UP TO REDSHIFT = 1.5,” Astrophys. J., vol. 817, no. 1, p. 20, Jan. 2016, doi: 10.3847/0004-637X/817/1/20

    2016 doi

  17. [24]

    A ~50,000 M$_{⊙}$ Solar Mass Black Hole in the Nucleus of RGG 118,

    V. ~F. Baldassare, A. ~E. Reines, E. Gallo, and J. ~E. Greene, “A ~50,000 M$_{⊙}$ Solar Mass Black Hole in the Nucleus of RGG 118,” Astrophys. J.l, vol. 809, p. L14, Aug. 2015, doi: 10.1088/2041-8205/809/1/L14

    2015 doi

  18. [25]

    The Runaway Growth of Intermediate‐ Mass Black Holes in Dense Star Clusters,

    S. F. Portegies Zwart and S. L. W. McMillan, “The Runaway Growth of Intermediate‐ Mass Black Holes in Dense Star Clusters,” Astrophys. J., vol. 576, no. 2, pp. 899–907, 2002, doi: 10.1086/341798

    2002 doi

  19. [26]

    Formation of massive black holes through runaway collisions in dense young star clusters,

    S. F. Portegies Zwart, H. Baumgardt, P. Hut, J. Makino, and S. L. W. McMillan, “Formation of massive black holes through runaway collisions in dense young star clusters,” Nature, vol. 428, no. 6984, pp. 724–726, 2004, doi: 10.1038/nature02448

    2004 doi

  20. [27]

    An Intermediate-Mass Black Hole in the Globular Cluster G1: Improved Significance from New Keck and Hubble Space Telescope Observations,

    K. Gebhardt, R. ~M. Rich, and L. C. Ho, “An Intermediate-Mass Black Hole in the Globular Cluster G1: Improved Significance from New Keck and Hubble Space Telescope Observations,” Astrophys. J., vol. 634, no. 2, pp. 1093–1102, Dec. 2005, doi: 10.1086/497023

    2005 doi

  21. [28]

    An intermediate-mass black hole in the centre of the globular cluster 47 Tucanae,

    B. Kızıltan, H. Baumgardt, and A. Loeb, “An intermediate-mass black hole in the centre of the globular cluster 47 Tucanae,” Nature, vol. 542, no. 7640, pp. 203–205, 2017, doi: 10.1038/nature21361

    2017 doi

  22. [29]

    M33: A Galaxy with No Supermassive Black Hole,

    K. Gebhardt et al., “M33: A Galaxy with No Supermassive Black Hole,” Astron. J., vol. 122, no. 5, pp. 2469–2476, 2001, doi: 10.1086/323481

    2001 doi

  23. [30]

    The Low End of the Supermassive Black Hole Mass Function: Constraining the Mass of a Nuclear Black Hole in NGC 205 via Stellar Kinematics,

    M. Valluri, L. Ferrarese, D. Merritt, and C. L. Joseph, “The Low End of the Supermassive Black Hole Mass Function: Constraining the Mass of a Nuclear Black Hole in NGC 205 via Stellar Kinematics,” Astrophys. J., vol. 628, no. 1, pp. 137–152, 2005, doi: 10.1086/430752

    2005 doi

  24. [31]

    The AGN Fraction in Dwarf Galaxies from eROSITA: First Results and Future Prospects,

    L. J. Latimer, A. E. Reines, A. Bogdan, and R. Kraft, “The AGN Fraction in Dwarf Galaxies from eROSITA: First Results and Future Prospects,” Astrophys. J. Lett., vol. 922, no. 2, p. L40, Dec. 2021, doi: 10.3847/2041-8213/ac3af6

    2021 doi

  25. [32]

    X-ray detected AGN in SDSS dwarf galaxies,

    K. L. Birchall, M. G. Watson, and J. Aird, “X-ray detected AGN in SDSS dwarf galaxies,” Mon. Not. R. Astron. Soc., vol. 492, no. 2, pp. 2268–2284, 2020, doi: 10.1093/mnras/staa040

    2020 doi

  26. [33]

    AN X-RAY- SELECTED SAMPLE OF CANDIDATE BLACK HOLES IN DWARF GALAXIES,

    S. M. Lemons, A. E. Reines, R. M. Plotkin, E. Gallo, and J. E. Greene, “AN X-RAY- SELECTED SAMPLE OF CANDIDATE BLACK HOLES IN DWARF GALAXIES,” Astrophys. J., vol. 805, no. 1, p. 12, May 2015, doi: 10.1088/0004-637X/805/1/12

    2015 doi

  27. [34]

    Exploring the Optical Transient Sky with the Palomar Transient Factory,

    A. Rau et al., “Exploring the Optical Transient Sky with the Palomar Transient Factory,” Publ. Astron. Soc. Pacific, vol. 121, no. 886, p. 1334, Oct. 2009, doi: 10.1086/605911

    2009 doi

  28. [35]

    The Palomar Transient Factory: System Overview, Performance, and First Results,

    N. M. Law et al., “The Palomar Transient Factory: System Overview, Performance, and First Results,” Publ. Astron. Soc. Pacific, vol. 121, no. 886, p. 1395, Nov. 2009, doi: 10.1086/648598

    2009 doi

  29. [36]

    The Zwicky Transient Facility: Science Objectives,

    M. J. Graham et al., “The Zwicky Transient Facility: Science Objectives,” Publ. Astron. Soc. Pacific, vol. 131, no. 1001, p. 78001, May 2019, doi: 10.1088/1538-3873/ab006c

    2019 doi

  30. [37]

    THE CALTECH-NRAO STRIPE 82 SURVEY (CNSS) PAPER. I. THE PILOT RADIO TRANSIENT SURVEY IN 50 DEG2,

    K. P. Mooley et al., “THE CALTECH-NRAO STRIPE 82 SURVEY (CNSS) PAPER. I. THE PILOT RADIO TRANSIENT SURVEY IN 50 DEG2,” Astrophys. J., vol. 818, no. 2, p. 105, Feb. 2016, doi: 10.3847/0004-637X/818/2/105

    2016 doi

  31. [38]

    Dynamical Constraints on the Masses of the Nuclear Star Cluster and Black Hole in the Late-Type Spiral Galaxy NGC 3621,

    A. J. Barth, L. E. Strigari, M. C. Bentz, J. E. Greene, and L. C. Ho, “Dynamical Constraints on the Masses of the Nuclear Star Cluster and Black Hole in the Late-Type Spiral Galaxy NGC 3621,” Astrophys. J., vol. 690, no. 1, pp. 1031–1044, Jan. 2009, doi: 10.1088/0004-637X/690/1/1031

    2009 doi

  32. [39]

    Measuring the mass of the central black hole in the bulgeless galaxy NGC 4395 from gas dynamical modeling,

    M. Den Brok et al., “Measuring the mass of the central black hole in the bulgeless galaxy NGC 4395 from gas dynamical modeling,” Astrophys. J., vol. 809, no. 1, p. 101, 2015, doi: 10.1088/0004-637X/809/1/101

    2015 doi

  33. [40]

    Nearby Early-type Galactic Nuclei at High Resolution: Dynamical Black Hole and Nuclear Star Cluster Mass Measurements,

    D. D. Nguyen et al., “Nearby Early-type Galactic Nuclei at High Resolution: Dynamical Black Hole and Nuclear Star Cluster Mass Measurements,” Astrophys. J., vol. 858, no. 2, p. 118, May 2018, doi: 10.3847/1538-4357/aabe28

    2018 doi

  34. [43]

    Improved Dynamical Constraints on the Mass of the Central Black Hole in NGC 404,

    D. D. Nguyen et al., “Improved Dynamical Constraints on the Mass of the Central Black Hole in NGC 404,” Astrophys. J., vol. 836, no. 2, p. 237, Feb. 2017, doi: 10.3847/1538-4357/aa5cb4

    2017 doi

  35. [44]

    Revealing the intermediate-mass black hole at the heart of the dwarf galaxy NGC 404 with sub-parsec resolution ALMA observations,

    T. A. Davis et al., “Revealing the intermediate-mass black hole at the heart of the dwarf galaxy NGC 404 with sub-parsec resolution ALMA observations,” Monthly Notices of the Royal Astronomical Society, vol. 496, no. 4, pp. 4061–4078, Jul. 2020, doi: 10.1093/mnras/staa1567

    2020 doi

  36. [45]

    Fast-moving stars around an intermediate-mass black hole in {\ensuremath{\omega}} Centauri,

    M. Häberle et al., “Fast-moving stars around an intermediate-mass black hole in {\ensuremath{\omega}} Centauri,” Nature, vol. 631, no. 8020, pp. 285–288, Jul. 2024, doi: 10.1038/s41586-024-07511-z

    2024 doi

  37. [46]

    Detection of a 100,000 M $_{{\ensuremath{\odot}}}$ black hole in M31’s Most Massive Globular Cluster: A Tidally Stripped Nucleus,

    R. Pechetti et al., “Detection of a 100,000 M $_{{\ensuremath{\odot}}}$ black hole in M31’s Most Massive Globular Cluster: A Tidally Stripped Nucleus,” Astrophys. J., vol. 924, no. 2, p. 48, Jan. 2022, doi: 10.3847/1538-4357/ac339f

    2022 doi

  38. [47]

    D. D. Nguyen et al., “Simulating intermediate black hole mass measurements for a sample of galaxies with nuclear star clusters using ELT/HARMONI high spatial resolution integral-field stellar kinematics,” arXiv e-prints, p. arXiv:2408.00239, Jul. 2024, doi: 10.48550/arXiv.2408.00239

    2024 doi arXiv

  39. [48]

    Studies of the Virgo Cluster. VI. Morphological and Kinematical Structure of the Virgo Cluster,

    B. Binggeli, G. ~A. Tammann, and A. Sandage, “Studies of the Virgo Cluster. VI. Morphological and Kinematical Structure of the Virgo Cluster,” \aj, vol. 94, p. 251, Aug. 1987, doi: 10.1086/114467

    1987 doi

  40. [50]

    Expected intermediate-mass black holes in the Virgo cluster – II. Late-type galaxies,

    A. W. Graham, R. Soria, and B. L. Davis, “Expected intermediate-mass black holes in the Virgo cluster – II. Late-type galaxies,” Mon. Not. R. Astron. Soc., vol. 484, no. 1, pp. 814–831, 2018, doi: 10.1093/mnras/sty3068

    2018 doi

  41. [51]

    Galaxy Populations in the Fornax and Virgo Clusters,

    H. C. Ferguson, “Galaxy Populations in the Fornax and Virgo Clusters,” \apss, vol. 157, no. 1–2, pp. 227–233, Jul. 1989, doi: 10.1007/BF00637334

    1989 doi

  42. [52]

    Virgo Redux: The Masses and Stellar Content of Nuclei in Early- type Galaxies from Multiband Photometry and Spectroscopy,

    C. Spengler et al., “Virgo Redux: The Masses and Stellar Content of Nuclei in Early- type Galaxies from Multiband Photometry and Spectroscopy,” Astrophys. J., vol. 849, no. 1, p. 55, Nov. 2017, doi: 10.3847/1538-4357/aa8a78

    2017 doi

  43. [53]

    UPDATED MASS SCALING RELATIONS FOR NUCLEAR STAR CLUSTERS AND A COMPARISON TO SUPERMASSIVE BLACK HOLES,

    N. Scott and A. W. Graham, “UPDATED MASS SCALING RELATIONS FOR NUCLEAR STAR CLUSTERS AND A COMPARISON TO SUPERMASSIVE BLACK HOLES,” Astrophys. J., vol. 763, no. 2, p. 76, Jan. 2013, doi: 10.1088/0004- 637X/763/2/76

    2013 doi

  44. [54]

    Toloba et al., “STELLAR KINEMATICS AND STRUCTURAL PROPERTIES OF VIRGO CLUSTER DWARF EARLY-TYPE GALAXIES FROM THE SMAKCED PROJECT

    E. Toloba et al., “STELLAR KINEMATICS AND STRUCTURAL PROPERTIES OF VIRGO CLUSTER DWARF EARLY-TYPE GALAXIES FROM THE SMAKCED PROJECT. II. THE SURVEY AND A SYSTEMATIC ANALYSIS OF KINEMATIC ANOMALIES AND ASYMMETRIES,” Astrophys. J. Suppl. Ser., vol. 215, no. 2, p. 17, Dec. 2014, ...

    2014 doi

  45. [55]

    The hELENa project – I. Stellar populations of early-type galaxies linked with local environment and galaxy mass,

    A. Sybilska et al., “The hELENa project – I. Stellar populations of early-type galaxies linked with local environment and galaxy mass,” Mon. Not. R. Astron. Soc., vol. 470, no. 1, pp. 815–838, 2017, doi: 10.1093/mnras/stx1138

    2017 doi

  46. [56]

    Detailed Surface Photometry of Dwarf Elliptical and Dwarf S0 Galaxies in the Virgo Cluster,

    B. S. Ryden, D. M. Terndrup, R. W. Pogge, and T. R. Lauer, “Detailed Surface Photometry of Dwarf Elliptical and Dwarf S0 Galaxies in the Virgo Cluster,” Astrophys. J., vol. 517, no. 2, p. 650, Jun. 1999, doi: 10.1086/307201

    1999 doi

  47. [57]

    The ACS Virgo Cluster Survey. VIII. The Nuclei of Early-Type Galaxies,

    P. Côté et al., “The ACS Virgo Cluster Survey. VIII. The Nuclei of Early-Type Galaxies,” Astrophys. J.s, vol. 165, no. 1, pp. 57–94, Jul. 2006, doi: 10.1086/504042

    2006 doi

  48. [58]

    hsim: a simulation pipeline for the HARMONI integral field spectrograph on the European ELT,

    S. Zieleniewski et al., “hsim: a simulation pipeline for the HARMONI integral field spectrograph on the European ELT,” Mon. Not. R. Astron. Soc., vol. 453, no. 4, pp. 3754–3765, Nov. 2015, doi: 10.1093/mnras/stv1860

    2015 doi

  49. [59]

    Simulation of HST PSFs using Tiny Tim,

    J. Krist, “Simulation of HST PSFs using Tiny Tim,” in Astronomical Data Analysis Software and Systems IV, Jan. 1995, vol. 77, p. 349

    1995

  50. [60]

    20 years of Hubble Space Telescope optical modeling using Tiny Tim,

    J. E. Krist, R. N. Hook, and F. Stoehr, “20 years of Hubble Space Telescope optical modeling using Tiny Tim,” in Optical Modeling and Performance Predictions V, Oct. 2011, vol. 8127, p. 81270J, doi: 10.1117/12.892762

    2011 doi

  51. [61]

    AstroDrizzle: Aligning Images From Multiple Instruments,

    R. J. Avila, W. ~J. Hack, and STScI AstroDrizzle Team, “AstroDrizzle: Aligning Images From Multiple Instruments,” in American Astronomical Society Meeting Abstracts \#220, May 2012, vol. 220, p. 135.13

    2012

  52. [62]

    CCD surface photometry of elliptical galaxies - I. Observations, reduction and results.,

    R. I. Jedrzejewski, “CCD surface photometry of elliptical galaxies - I. Observations, reduction and results.,” Monthly Notices of the Royal Astronomical Society, vol. 226, pp. 747–768, Jun. 1987, doi: 10.1093/mnras/226.4.747

    1987 doi

  53. [63]

    A New Empirical Model for the Structural Analysis of Early-Type Galaxies, and A Critical Review of the Nuker Model,

    A. W. Graham, P. Erwin, I. Trujillo, and A. Asensio Ramos, “A New Empirical Model for the Structural Analysis of Early-Type Galaxies, and A Critical Review of the Nuker Model,” \aj, vol. 125, pp. 2951–2963, Jun. 2003, doi: 10.1086/375320

    2003 doi

  54. [64]

    Evidence for a New Elliptical-Galaxy Paradigm: Sérsic and Core Galaxies,

    I. Trujillo, P. Erwin, A. Asensio Ramos, and A. W. Graham, “Evidence for a New Elliptical-Galaxy Paradigm: Sérsic and Core Galaxies,” \aj, vol. 127, pp. 1917–1942, Apr. 2004, doi: 10.1086/382712

    1917 doi

  55. [65]

    J. L. Sersic, Atlas de galaxias australes. Córdoba: Obs. Astron. Univ. Nacional de Córdoba, 1968

    1968

  56. [66]

    Non-linear Least-squares Fitting in IDL with MPFIT,

    C. ~B. Markwardt, “Non-linear Least-squares Fitting in IDL with MPFIT,” in Astronomical Data Analysis Software and Systems XVIII, Sep. 2009, vol. 411, p. 251, doi: 10.48550/arXiv.0902.2850

    2009 doi arXiv

  57. [67]

    van de Sande, M

    J. van de Sande, M. Kriek, M. Franx, R. Bezanson, and P. G. van Dokkum, “The Relation between Dynamical Mass-to-light Ratio and Color for Massive Quiescent Galaxies out to z \raisebox{-0.5ex}\textasciitilde 2 and Comparison with Stellar Population Synthesis Models,” Astrophys....

    2015 doi

  58. [68]

    Stellar population models at high spectral resolution,

    C. Maraston and G. Strömbäck, “Stellar population models at high spectral resolution,” Monthly Notices of the Royal Astronomical Society, vol. 418, no. 4, pp. 2785–2811, Dec. 2011, doi: 10.1111/j.1365-2966.2011.19738.x

    2011

  59. [69]

    A grid of MARCS model atmospheres for late-type stars. I. Methods and general properties,

    B. Gustafsson, B. Edvardsson, K. Eriksson, U. ~G. Jørgensen, \rA. Nordlund, and B. Plez, “A grid of MARCS model atmospheres for late-type stars. I. Methods and general properties,” \aap, vol. 486, no. 3, pp. 951–970, Aug. 2008, doi: 10.1051/0004- 6361:200809724

    2008 doi

  60. [70]

    The Coincidence of Nuclear Star Clusters and Active Galactic Nuclei,

    A. Seth, M. Agüeros, D. Lee, and A. Basu-Zych, “The Coincidence of Nuclear Star Clusters and Active Galactic Nuclei,” Astrophys. J., vol. 678, no. 1, pp. 116–130, May 2008, doi: 10.1086/528955

    2008 doi

  61. [71]

    Measuring the inclination and mass-to-light ratio of axisymmetric galaxies via anisotropic Jeans models of stellar kinematics,

    M. Cappellari, “Measuring the inclination and mass-to-light ratio of axisymmetric galaxies via anisotropic Jeans models of stellar kinematics,” Mon. Not. R. Astron. Soc., vol. 390, no. 1, pp. 71–86, Oct. 2008, doi: 10.1111/j.1365-2966.2008.13754.x

    2008

  62. [72]

    Efficient solution of the anisotropic spherically aligned axisymmetric Jeans equations of stellar hydrodynamics for galactic dynamics,

    M. Cappellari, “Efficient solution of the anisotropic spherically aligned axisymmetric Jeans equations of stellar hydrodynamics for galactic dynamics,” Mon. Not. R. Astron. Soc., vol. 494, no. 4, pp. 4819–4837, Jun. 2020, doi: 10.1093/mnras/staa959

    2020 doi

  63. [73]

    The VIRUS-dE Survey I: Stars in dwarf elliptical galaxies - 3D dynamics and radially resolved stellar initial mass functions

    M. Lipka et al., “The VIRUS-dE Survey I: Stars in dwarf elliptical galaxies - 3D dynamics and radially resolved stellar initial mass functions.” 2024, [Online]. Available: https://arxiv.org/abs/2409.10518

    2024 arXiv

  64. [74]

    The E-ELT first light spectrograph HARMONI: capabilities and modes,

    N. A. Thatte et al., “The E-ELT first light spectrograph HARMONI: capabilities and modes,” in Ground-based and Airborne Instrumentation for Astronomy VI, Aug. 2016, vol. 9908, p. 99081X, doi: 10.1117/12.2230629

    2016 doi

  65. [75]

    Simulating supermassive black hole mass measurements for a sample of ultramassive galaxies using ELT/HARMONI high-spatial-resolution integral-field stellar kinematics,

    D. D. Nguyen, M. Cappellari, and M. Pereira-Santaella, “Simulating supermassive black hole mass measurements for a sample of ultramassive galaxies using ELT/HARMONI high-spatial-resolution integral-field stellar kinematics,” Monthly Notices of the Royal Astronomical Society, v...

    2023 doi

  66. [76]

    Simulated stellar kinematics studies of high-redshift galaxies with the HARMONI Integral Field Spectrograph,

    S. Kendrew et al., “Simulated stellar kinematics studies of high-redshift galaxies with the HARMONI Integral Field Spectrograph,” Mon. Not. R. Astron. Soc., vol. 458, no. 3, pp. 2405–2422, 2016, doi: 10.1093/mnras/stw438

    2016 doi

  67. [77]

    Near-infrared spectroscopy of stellar populations in nearby spiral galaxies,

    J. ~K. Kotilainen, T. Hyvönen, J. Reunanen, and V. ~D. Ivanov, “Near-infrared spectroscopy of stellar populations in nearby spiral galaxies,” Monthly Notices of the Royal Astronomical Society, vol. 425, no. 2, pp. 1057–1067, Sep. 2012, doi: 10.1111/j.1365-2966.2012.21425.x

    2012

  68. [78]

    Integrated J- and H-band spectra of globular clusters in the LMC: implications for stellar population models and galaxy age dating,

    M. Lyubenova, H. Kuntschner, M. Rejkuba, D. ~R. Silva, M. Kissler-Patig, and L. ~E. Tacconi-Garman, “Integrated J- and H-band spectra of globular clusters in the LMC: implications for stellar population models and galaxy age dating,” \aap, vol. 543, p. A75, Jul. 2012, doi: 10....

    2012 doi

  69. [79]

    Adaptive spatial binning of integral-field spectroscopic data using Voronoi tessellations,

    M. Cappellari and Y. Copin, “Adaptive spatial binning of integral-field spectroscopic data using Voronoi tessellations,” Monthly Notices of the Royal Astronomical Society, vol. 342, no. 2, pp. 345–354, Jun. 2003, doi: 10.1046/j.1365-8711.2003.06541.x

    2003

  70. [80]

    M. Cappellari, “Full spectrum fitting with photometry in PPXF: stellar population versus dynamical masses, non-parametric star formation history and metallicity for 3200 LEGA-C galaxies at redshift z {\ensuremath{\approx}} 0.8,” Monthly Notices of the Royal Astronomical Societ...

    2023 doi

  71. [81]

    A Family of Models for Spherical Stellar Systems,

    S. Tremaine et al., “A Family of Models for Spherical Stellar Systems,” Astron. J., vol. 107, p. 634, Feb. 1994, doi: 10.1086/116883

    1994 doi

  72. [82]

    The ATLAS3D project – XV. Benchmark for early-type galaxies scaling relations from 260 dynamical models: mass-to-light ratio, dark matter, Fundamental Plane and Mass Plane,

    M. Cappellari et al., “The ATLAS3D project – XV. Benchmark for early-type galaxies scaling relations from 260 dynamical models: mass-to-light ratio, dark matter, Fundamental Plane and Mass Plane,” Mon. Not. R. Astron. Soc., vol. 432, no. 3, pp. 1709–1741, Jul. 2013, doi: 10.10...

    2013 doi

Pith tools

Reviewed August 5, 2026 · model on record in the stance chip above.