THE SLOPE OF THE BARYONIC TULLY-FISHER RELATION

Journal Article · Wed Sep 15 04:00:00 EDT 2010 · Astronomical Journal (New York, N.Y. Online)

DOI:https://doi.org/10.1088/0004-6256/140/3/663· OSTI ID:21443249

Gurovich, Sebastian; Freeman, Kenneth; Jerjen, Helmut ^[1]; Staveley-Smith, Lister ^[2]; Puerari, Ivanio ^[3]

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1. Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston, ACT 2611 (Australia)
2. International Centre for Radio Astronomy Research, M468, University of Western Australia, 35 Sterling Highway, Crawley, WA 6009 (Australia)
3. Instituto Nacional de Astrofisica, Optica y Electronica, Calle Luis Enrique Erro 1, 72840 Santa MarIa Tonantzintla, Puebla (Mexico)

We present the results of a baryonic Tully-Fisher relation (BTFR) study for a local sample of relatively isolated disk galaxies. We derive a BTFR with a slope near 3 measured over about 4 dex in baryon mass for our combined H I and bright spiral disk samples. This BTFR is significantly flatter and has less scatter than the TFR (stellar mass only) with its slope near 4 reported for other samples and studies. A BTFR slope near 3 is in better agreement with the expected slope from simple {Lambda}CDM cosmological simulations that include both stellar and gas baryons. The scatter in the TFR/BTFR appears to depend on W{sub 20}: galaxies that rotate slower have more scatter. The atomic gas-to-stars ratio shows a break near W{sub 20} = 250 km s{sup -1} probably associated with a change in star formation efficiency. In contrast, the absence of such a break in the BTFR suggests that this relation was probably set at the main epoch of baryon dissipation rather than as a product of later galactic evolution.

• OSTI ID: 21443249
• Journal Information: Astronomical Journal (New York, N.Y. Online), Journal Name: Astronomical Journal (New York, N.Y. Online) Journal Issue: 3 Vol. 140; ISSN 1538-3881
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
BARYONS
COSMOLOGY
ELEMENTARY PARTICLES
EVOLUTION
FERMIONS
GALACTIC EVOLUTION
GALAXIES
HADRONS
MASS
MATTER
NONLUMINOUS MATTER
SIMULATION
STARS