Infrared Surface Brightness Fluctuation Distances for MASSIVE and Type Ia Supernova Host Galaxies*

Jensen, Joseph B.; Blakeslee, John P.; Ma, Chung‐Pei; Milne, Peter; Brown, P. J.; Cantiello, M.; Garnavich, P.; Greene, Jenny E.; Lucey, J. R.; Phan, A.; Tully, R. Brent; Wood, Charlotte

doi:10.3847/1538-4365/ac01e7

Cited by 28 publications

(69 citation statements)

References 82 publications

(144 reference statements)

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“…We adopt distances for 19 galaxies in our sample based on infrared surface brightness fluctuation measurement from Jensen et al (2021). In addition, we utilize galaxy properties measured in previous MASSIVE Survey papers (Ma et al 2014;Veale et al 2018;Ene et al 2020), including distances for other galaxies in the sample, foreground galactic extinction, and K-band photometry.…”

Section: Data Collectionmentioning

confidence: 99%

The MASSIVE SURVEY XVI. The Stellar Initial Mass Function in the Center of MASSIVE Early-Type Galaxies

Gu,

Greene,

Newman

et al. 2021

Preprint

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The stellar initial mass function (IMF) is a fundamental property in the measurement of stellar masses and galaxy star formation histories. In this work we focus on the most massive galaxies in the nearby universe log(M /M ) > 11.2. We obtain high quality Magellan/LDSS-3 long slit spectroscopy with a wide wavelength coverage of 0.4µm − 1.01µm for 41 early-type galaxies (ETGs) in the MASSIVE survey, and derive high S/N spectra within an aperture of R e /8. Using detailed stellar synthesis models, we constrain the elemental abundances and stellar IMF of each galaxy through full spectral modeling. All the ETGs in our sample have an IMF that is steeper than a Milky Way (Kroupa) IMF. The best-fit IMF mismatch parameter, α IMF = (M/L)/(M/L) MW , ranges from 1.12 to 3.05, with an average of α IMF = 1.84, suggesting that on average, the IMF is more bottomheavy than Salpeter. Comparing the estimated stellar mass with the dynamical mass, we find that most galaxies have stellar masses smaller than their dynamical masses within the 1σ uncertainty. We complement our sample with lower-mass galaxies from the literature, and confirm that log(α IMF ) is positively correlated with log(σ), log(M ), and log(M dyn ). The IMF in the centers of more massive ETGs is more bottom-heavy. In addition, we find that log(α IMF ) is positively correlated with both [Mg/Fe] and the estimated total metallicity [Z/H]. We find suggestive evidence that the effective stellar surface density Σ Kroupa might be responsible for the variation of α IMF . We conclude that σ, [Mg/Fe] and [Z/H] are the primary drivers of the global stellar IMF variation.

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Section: Data Collectionmentioning

confidence: 99%

The MASSIVE SURVEY XVI. The Stellar Initial Mass Function in the Center of MASSIVE Early-Type Galaxies

Gu,

Greene,

Newman

et al. 2021

Preprint

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“…In comparison, Cepheid calibrators must be within about 40 Mpc to obtain reliable measurements. Further, IR SBF measurements require only 1 to 2 Hubble Space Telescope (HST ) orbits per galaxy (Jensen et al 2021) to achieve a 5% distance precision. This can be compared with the more than 1000 total HST orbits needed to calibrate 42 SNe Ia hosts using Cepheid variables (Riess et al 2021).…”

Section: Introductionmentioning

confidence: 99%

“…The application of SBF to cosmologically interesting distances was demonstrated by Jensen et al (2001) using space-based, near-infrared (IR) imaging. Most recently, HST's Wide Field Camera 3 (WFC3) has proven to be a superb instrument for SBF distance calibrations, allowing for a median 3.9% distance uncertainty on 63 massive elliptical galaxy distances out to 100 Mpc (Jensen et al 2021).…”

Section: Introductionmentioning

confidence: 99%

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Connecting Infrared Surface Brightness Fluctuation Distances to Type Ia Supernova Hosts: Testing the Top Rung of the Distance Ladder

Garnavich¹,

Wood²,

Milne³

et al. 2022

Preprint

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We compare infrared surface brightness fluctuation (IR SBF) distances measured in galaxies that have hosted type Ia supernovae (SNe Ia) to distances estimated from SNe Ia light curve fits. We show that the properties of SNe Ia found in IR-SBF hosts are very different from those exploding in Cepheid calibrators, therefore, this is a direct test of systematic uncertainties on estimation of the Hubble-Lemaître constant (H 0 ) using supernovae. The IR SBF results from Jensen et al. ( 2021) provide a large and uniformly measured sample of IR SBF distances which we directly compare with distances to 25 SNe Ia host galaxies. We divide the Hubble flow SNe Ia into sub-samples that best match the divergent supernova properties seen in the IR SBF hosts and Cepheid hosts. We further divide the SNe Ia into a sample with light curve widths and host masses that are congruent to those found in the SBF-calibrated hosts. We refit the light curve stretch and color correlations with luminosity, and use these revised parameters to calibrate the Hubble flow SNe Ia with IR SBF calibrators. Relative to the Hubble flow, the average calibrator distance moduli vary by 0.03 mag depending on the SNe Ia subsamples examined and this adds a 1.8% systematic uncertainty to our Hubble-Lemaître constant estimate. Based on the IR SBF calibrators, H 0 = 74.6 ± 0.9(stat)±2.7(syst) km s −1 Mpc −1 , which is consistent with the Hubble-Lemaître constant derived from SNe Ia calibrated from Cepheid variables. We conclude that IR SBF provides reliable calibration of SNe Ia with a precision comparable to Cepheid calibrators, and with a significant saving in telescope time.

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“…We adopt a distance to NGC 2693 of 71.0 Mpc from the MASSIVE-WFC3 project (Goullaud et al 2018) using the surface-brightness fluctuation technique (Jensen et al 2021;Blakeslee et al 2021). At this distance, 1 is 354 pc, assuming a flat ΛCDM cosmology with a matter density of Ω m = 0.315 and a Hubble parameter of H 0 = 70 km s −1 Mpc −1 .…”

Section: Introductionmentioning

confidence: 99%

The MASSIVE Survey -- XVII. A Triaxial Orbit-based Determination of the Black Hole Mass and Intrinsic Shape of Elliptical Galaxy NGC 2693

Pilawa,

Liepold,

Andrade

et al. 2021

Preprint

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We present a stellar dynamical mass measurement of a newly detected supermassive black hole (SMBH) at the center of the fast-rotating, massive elliptical galaxy NGC 2693 as part of the MASSIVE survey. We combine high signal-to-noise integral field spectroscopy (IFS) from the Gemini Multi-Object Spectrograph (GMOS) with wide-field data from the Mitchell Spectrograph at McDonald Observatory to extract and model stellar kinematics of NGC 2693 from the central ∼ 150 pc out to ∼ 2.5 effective radii. Observations from Hubble Space Telescope (HST ) WFC3 are used to determine the stellar light distribution. We perform fully triaxial Schwarzschild orbit modeling using the latest TriOS code, and search a 6-D galaxy model parameter space to determine NGC 2693's SMBH mass (M BH ), stellar mass-to-light ratio, dark matter content, and intrinsic shape. We find M BH = (1.7 ± 0.4) × 10 9 M and a triaxial intrinsic shape with axis ratios p = b/a = 0.902 ± 0.009 and q = c/a = 0.721 +0.011 −0.010 , triaxiality parameter T = 0.39 ± 0.04. In comparison, the best-fit axisymmetric orbit model and Jeans anisotropic model of NGC 2693 prefer a 40% and 75% larger M BH , respectively, and neither model can account for the non-axisymmetric stellar velocity features present in the IFS data.

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Infrared Surface Brightness Fluctuation Distances for MASSIVE and Type Ia Supernova Host Galaxies*

Cited by 28 publications

References 82 publications

The MASSIVE SURVEY XVI. The Stellar Initial Mass Function in the Center of MASSIVE Early-Type Galaxies

The MASSIVE SURVEY XVI. The Stellar Initial Mass Function in the Center of MASSIVE Early-Type Galaxies

Connecting Infrared Surface Brightness Fluctuation Distances to Type Ia Supernova Hosts: Testing the Top Rung of the Distance Ladder

The MASSIVE Survey -- XVII. A Triaxial Orbit-based Determination of the Black Hole Mass and Intrinsic Shape of Elliptical Galaxy NGC 2693

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