Dark matter halos and scaling relations of extremely massive spiral galaxies from extended HI rotation curves. (arXiv:2207.02906v2 [astro-ph.GA] UPDATED)

Dark matter halos and scaling relations of extremely massive spiral galaxies from extended HI rotation curves. (arXiv:2207.02906v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Teodoro_E/0/1/0/all/0/1">Enrico M. Di Teodoro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Posti_L/0/1/0/all/0/1">Lorenzo Posti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fall_S/0/1/0/all/0/1">S. Michael Fall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ogle_P/0/1/0/all/0/1">Patrick M. Ogle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jarrett_T/0/1/0/all/0/1">Thomas Jarrett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Appleton_P/0/1/0/all/0/1">Philip N. Appleton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cluver_M/0/1/0/all/0/1">Michelle E. Cluver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haynes_M/0/1/0/all/0/1">Martha P. Haynes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lisenfeld_U/0/1/0/all/0/1">Ute Lisenfeld</a>

We present new and archival atomic hydrogen (hi) observations of galnum of
the most massive spiral galaxies in the local Universe ($M_star>10^{11} ,
mathrm{M}_odot$). From 3D kinematic modeling of the datacubes, we derive
extended hi rotation curves, and from these, we estimate masses of the dark
matter halos and specific angular momenta of the discs. We confirm that massive
spiral galaxies lie at the upper ends of the Tully-Fisher relation (mass vs
velocity, $M propto V^{4}$) and Fall relation (specific angular momentum vs
mass, $j propto M^{0.6}$), in both stellar and baryonic forms, with no
significant deviations from single power laws. We study the connections between
baryons and dark matter through the stellar (and baryon)-to-halo ratios of mass
$f_mathrm{M} equiv M_star/M_mathrm{h}$ and specific angular momentum
$f_mathrm{j} equiv j_star/j_mathrm{h}$ and $f_mathrm{j,bar} equiv
j_mathrm{bar}/j_mathrm{h}$. Combining our sample with others from the
literature for less massive disc-dominated galaxies, we find that
$f_mathrm{M}$ rises monotonically with $M_star$ and $M_mathrm{h}$ (instead
of the inverted-U shaped $f_mathrm{M}$ for spheroid-dominated galaxies), while
$f_mathrm{j}$ and $f_mathrm{j,bar}$ are essentially constant near unity over
four decades in mass. Our results indicate that disc galaxies constitute a
self-similar population of objects closely linked to the self-similarity of
their dark halos. This picture is reminiscent of early analytical models of
galaxy formation wherein discs grow by relatively smooth and gradual inflow,
isolated from disruptive events such as major mergers and strong AGN feedback,
in contrast to the more chaotic growth of spheroids.

We present new and archival atomic hydrogen (hi) observations of galnum of
the most massive spiral galaxies in the local Universe ($M_star>10^{11} ,
mathrm{M}_odot$). From 3D kinematic modeling of the datacubes, we derive
extended hi rotation curves, and from these, we estimate masses of the dark
matter halos and specific angular momenta of the discs. We confirm that massive
spiral galaxies lie at the upper ends of the Tully-Fisher relation (mass vs
velocity, $M propto V^{4}$) and Fall relation (specific angular momentum vs
mass, $j propto M^{0.6}$), in both stellar and baryonic forms, with no
significant deviations from single power laws. We study the connections between
baryons and dark matter through the stellar (and baryon)-to-halo ratios of mass
$f_mathrm{M} equiv M_star/M_mathrm{h}$ and specific angular momentum
$f_mathrm{j} equiv j_star/j_mathrm{h}$ and $f_mathrm{j,bar} equiv
j_mathrm{bar}/j_mathrm{h}$. Combining our sample with others from the
literature for less massive disc-dominated galaxies, we find that
$f_mathrm{M}$ rises monotonically with $M_star$ and $M_mathrm{h}$ (instead
of the inverted-U shaped $f_mathrm{M}$ for spheroid-dominated galaxies), while
$f_mathrm{j}$ and $f_mathrm{j,bar}$ are essentially constant near unity over
four decades in mass. Our results indicate that disc galaxies constitute a
self-similar population of objects closely linked to the self-similarity of
their dark halos. This picture is reminiscent of early analytical models of
galaxy formation wherein discs grow by relatively smooth and gradual inflow,
isolated from disruptive events such as major mergers and strong AGN feedback,
in contrast to the more chaotic growth of spheroids.

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