The slope of the baryonic tully-fisher relation

Sebastín Gurovich; Kenneth Freeman; Helmut Jerjen; Lister Staveley-Smith; Ivânid Puerari

doi:10.1088/0004-6256/140/3/663

The slope of the baryonic tully-fisher relation

Sebastín Gurovich^*, Kenneth Freeman, Helmut Jerjen, Lister Staveley-Smith, Ivânid Puerari

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

53 Citations (Scopus)

Abstract

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 HI 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 ACDM cosmological simulations that include both stellar and gas baryons. The scatter in the TFR/BTFR appears to depend on W ₂₀: galaxies that rotate slower have more scatter. The atomic gas-to-stars ratio shows a break near W₂₀ = 250 km s-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.

Original language	English
Pages (from-to)	663-676
Number of pages	14
Journal	Astronomical Journal
Volume	140
Issue number	3
DOIs	https://doi.org/10.1088/0004-6256/140/3/663
Publication status	Published - Sept 2010

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title = "The slope of the baryonic tully-fisher relation",

abstract = "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 HI 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 ACDM cosmological simulations that include both stellar and gas baryons. The scatter in the TFR/BTFR appears to depend on W 20: galaxies that rotate slower have more scatter. The atomic gas-to-stars ratio shows a break near W20 = 250 km s-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.",

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T1 - The slope of the baryonic tully-fisher relation

AU - Gurovich, Sebastín

AU - Freeman, Kenneth

AU - Jerjen, Helmut

AU - Staveley-Smith, Lister

AU - Puerari, Ivânid

PY - 2010/9

Y1 - 2010/9

N2 - 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 HI 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 ACDM cosmological simulations that include both stellar and gas baryons. The scatter in the TFR/BTFR appears to depend on W 20: galaxies that rotate slower have more scatter. The atomic gas-to-stars ratio shows a break near W20 = 250 km s-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.

AB - 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 HI 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 ACDM cosmological simulations that include both stellar and gas baryons. The scatter in the TFR/BTFR appears to depend on W 20: galaxies that rotate slower have more scatter. The atomic gas-to-stars ratio shows a break near W20 = 250 km s-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.

KW - Cosmology

KW - Dark matter

KW - Evolution

KW - Formation

KW - Galaxies

KW - Observations

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DO - 10.1088/0004-6256/140/3/663

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VL - 140

SP - 663

EP - 676

JO - Astronomical Journal

JF - Astronomical Journal

IS - 3

ER -

The slope of the baryonic tully-fisher relation

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