GHASP: an H α kinematics survey of spiral galaxies – XII. Distribution of luminous and dark matter in spiral and irregular nearby galaxies using Rc-band photometry

Korsaga, Marie; Amram, P.; Carignan, C.; Épinat, B.

doi:10.1093/mnras/sty2582

Cited by 9 publications

(11 citation statements)

References 48 publications

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“…About 100 RCs of the above quality have been thoroughly investigated so far, and the results have led to a similar decisive support in favor of the DM halo cored distribution (e.g., Adams et al 2012;Donato et al 2009;Weinberg et al 2015;Simon et al 2005;de Blok & Bosma 2002;Spekkens et al 2005). The current status of the analysis of individual RCs is described in Korsaga et al (2018Korsaga et al ( , 2019a, who obtained mass models of 31 spiral and irregular galaxies, derived using hybrid rotation curves that combined high-resolution optical GHASP Fabry-Perot Hα RCs with extended radio WHISP HI RCs. A&A 643, A161 (2020) Moreover, for each galaxy, the analysis took advantage of highquality 3.4 µm WISE photometry, which is a fair indicator of the stellar disk mass.…”

Section: Introductionmentioning

confidence: 90%

Navarro-Frenk-White dark matter profile and the dark halos around disk systems

Dehghani

Salucci

Ghaffarnejad

2020

A&A

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Context. The Λ cold dark matter (ΛCDM) scenario is able to describe the Universe at large scales, but clearly shows some serious difficulties at small scales. The core-cusp question is one of these difficulties: the inner dark matter (DM) density profiles of spiral galaxies generally appear to be cored, without the r−1 profile that is predicted by N-body simulations in the above scenario. Aims. It is well known that in a more physical context, the baryons in the galaxy might backreact and erase the original cusp through supernova explosions. Before the efficiency and the presence of this effect is investigated, it is important to determine how wide and frequent the discrepancy between observed and N-body-predicted profiles is and what its features are. Methods. We used more than 3200 quite extended rotation curves (RCs) of good quality and high resolution of disk systems that included normal and dwarf spirals as well as low surface brightness galaxies. The curves cover all magnitude ranges. All these RCs were condensed into 26 coadded RCs, each of them built with individual RCs of galaxies of similar luminosity and morphology. We performed mass models of these 26 RCs using the Navarro-Frenk-White (NFW) profile for the contribution of the DM halo to the circular velocity and the exponential Freeman disk for the contribution of the stellar disk. Results. The fits are generally poor in all the 26 cases: in several cases, we find χred2 > 2. Moreover, the best-fitting values of three parameters of the model (c, MD, and Mvir) combined with those of their 1σ uncertainty clearly contradict well-known expectations of the ΛCDM scenario. We also tested the scaling relations that exist in spirals with the outcome of the current mass modeling: the modeling does not account for these scaling relations. Conclusions. The results of testing the NFW profile in disk systems indicate that this DM halo density law cannot account for the kinematics of the whole family of disk galaxies. It is therefore mandatory for the success of the ΛCDM scenario in any disk galaxy of any luminosity or maximum rotational velocity to transform initial cusps into the observed cores.

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Section: Introductionmentioning

confidence: 90%

Navarro-Frenk-White dark matter profile and the dark halos around disk systems

Dehghani

Salucci

Ghaffarnejad

2020

A&A

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“…The infrared surface photometry provides smaller dispersion for the M/L ratios compared to the optical photometry (Korsaga et al 2019). Several models also predict that the values of the M/L ratios Cote et al 1991;Br92: Broeils 1992;VM97: Verdes-Montenegro et al 1997;Be91: Begeman et al 1991;Bo08: Boomsma et al 2008).…”

Section: Photometric Datamentioning

confidence: 96%

“…In previous papers, the mass distribution was first determined using Hα RCs with the stellar mass component (disc and bulge, if presence of a bulge). We looked at the differences when using the mid-IR W 1 photometric band (Korsaga et al 2018) vs the optical R c band (Korsaga et al 2019) data. Since we found in those studies that it was better to use mid-IR photometry, WISE W 1 data will be used in the rest of this study.…”

Section: Analysis Of the Mass Models For Individual Galaxiesmentioning

confidence: 99%

“…Korsaga et al (2018) in their work, used 121 Hα RCs combined to WISE W 1 -band photometric data to determine the DM halo distribution. Another study was also done using a sample of 100 Hα RCs combined with optical R c -band photometric data (Korsaga et al 2019). The main aim was to see if the luminous and DM parameters were dependant of the photometric band used (optical vs IR), since they are dominated by different stellar populations.…”

Section: Introductionmentioning

confidence: 99%

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GHASP: an H α kinematical survey of spiral galaxies – XI. Distribution of luminous and dark matter in spiral and irregular nearby galaxies using WISE photometry

Korsaga

Carignan

Amram

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present the mass models of 31 spiral and irregular nearby galaxies obtained using hybrid rotation curves (RCs) combining high resolution GHASP Fabry-Perot Hα RCs and extended WHISP H ones together with 3.4 µm WISE photometry. The aim is to compare the dark matter (DM) halo properties within the optical radius using only Hα RCs with the effect of including and excluding the mass contribution of the neutral gas component, and when using H or hybrid RCs. Pseudo-isothermal (ISO) core and Navarro-Frenk-White (NFW) cuspy DM halo profiles are used with various fiducial fitting procedures. Mass models using Hα RCs including or excluding the H gas component provide compatible disc M/L. The correlations between DM halo and baryon parameters do not strongly depend on the RC. Clearly, the differences between the fitting procedures are larger than between the different datasets. Hybrid and H RCs lead to higher M/L values for both ISO and NFW best fit models but lower central densities for ISO halos and higher concentration for NFW halos than when using Hα RCs only. The agreement with the mass model parameters deduced using hybrid RCs, considered as a reference, is better for H than for Hα RCs. ISO density profiles better fit the RCs than the NFW ones, especially when using Hα or hybrid RCs. Halo masses at the optical radius determined using the various datasets are compatible even if they tend to be overestimated with Hα RCs. Hybrid RCs are thus ideal to study the mass distribution within the optical radius.

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“…3. Korsaga et al (2019). Finally, we use a model to fit V max rather than fitting the raw rotation curve, precisely to average local noncircular motions.…”

Section: Kinematical Projection Parametersmentioning

confidence: 99%

An Hα kinematic survey of the Herschel Reference Survey

Gómez-López

Amram

Épinat

et al. 2019

A&A

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Aims. We present new 2D high resolution Fabry–Perot spectroscopic observations of 152 star-forming galaxies that are part of the Herschel Reference Survey (HRS), which is a complete K-band selected, volume-limited sample of nearby galaxies that spans a wide range of stellar mass and morphological types. Methods. By using improved data reduction techniques, that provide adaptive binning based on Voronoi tessellation, and using large field-of-view observations, we derived high spectral resolution (R > 10 000) Hα datacubes from which we computed Hα maps and radial 2D velocity fields that are based on several of thousand independent measurements. A robust method based on such fields allowed us to accurately compute rotation curves and kinematical parameters, for which uncertainties are calculated using a method based on the power spectrum of the residual velocity fields. Results. We checked the consistency of the rotation curves by comparing our maximum rotational velocities to those derived from H I data, and by computing the i-band, NIR, stellar, and baryonic Tully-Fisher relations. We used this set of kinematical data combined with those available at other frequencies to study, for the first time, the relation between the dynamical and the total baryonic mass (stars, atomic and molecular gas, metals, and dust) and to derive the baryonic and dynamical main sequence on a representative sample of the local universe.

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GHASP: an H α kinematics survey of spiral galaxies – XII. Distribution of luminous and dark matter in spiral and irregular nearby galaxies using Rc-band photometry

Cited by 9 publications

References 48 publications

Navarro-Frenk-White dark matter profile and the dark halos around disk systems

Navarro-Frenk-White dark matter profile and the dark halos around disk systems

GHASP: an H α kinematical survey of spiral galaxies – XI. Distribution of luminous and dark matter in spiral and irregular nearby galaxies using WISE photometry

An Hα kinematic survey of the Herschel Reference Survey

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