Constraints on intragroup stellar mass from hostless Type Ia supernovae

S.L. McGee; M.L. Balogh

doi:10.1111/j.1745-3933.2010.00819.x

Constraints on intragroup stellar mass from hostless Type Ia supernovae

S.L. McGee, M.L. Balogh

Physics and Astronomy

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

43 Citations (Scopus)

Abstract

We probe the diffuse stellar mass in a sample of 1401 low-redshift galaxy groups (1013-1014 h-1 M⊙) by examining the rate of hostless Type Ia supernovae (SNe Ia) within the groups. We correlate the sample of confirmed SNe Ia from the Sloan Digital Sky Survey SN survey with the positions of our galaxy groups, as well as with the resolved galaxies within them. We find that 19 of the 59 SNe Ia within the group sample have no detectable host galaxy, with another three ambiguous instances. This gives a robust upper limit that a maximum of 2.69+1.58-1.34 per cent of the group's total mass arises from diffuse stars in the intragroup medium. After correcting for a contribution from 'prompt' SNe occurring within galaxies, and including a contribution from those which arise in dwarf galaxies below our photometric limit, we find that only 1.32+0.78-0.70 per cent of the group's total mass is likely in the form of diffuse stellar mass. Combining this result with the galaxy stellar mass functions of Yang, Mo and van den Bosch, we find that 47+16-15 per cent of the stellar mass in our groups is in the form of diffuse light, so that stars make up a fraction 0.028+0.011-0.010 of the total group mass. Galaxy groups appear to be very efficient in disrupting stellar mass into a diffuse component; however, stars still make up a small fraction of the group mass, comparable to that seen in rich clusters. This remains a challenge to galaxy formation models. © 2010 The Authors. Journal compilation © 2010 RAS.

Original language	English
Pages (from-to)	L79-L83
Journal	Monthly Notices of the Royal Astronomical Society: Letters
Volume	403
Issue number	1
DOIs	https://doi.org/10.1111/j.1745-3933.2010.00819.x
Publication status	Published - 2010

Bibliographical note

Export Date: 15 August 2017

Correspondence Address: McGee, S.L.; Department of Physics and Astronomy, University of Waterloo, Waterloo, ON N2L 3G1, Canada; email: s2mcgee@uwaterloo.ca

References: Balogh, M.L., McCarthy, I.G., Bower, R.G., Eke, V.R., (2008) MNRAS, 385, p. 1003; Bazin, G., (2009) A&A, 499, p. 653; Berlind, A.A., (2006) ApJS, 167, p. 1; Berrier, J.C., (2009) ApJ, 690, p. 1292; Blanton, M.R., (2003) ApJ, 592, p. 819; Brinchmann, J., (2004) MNRAS, 351, p. 1151; Bullock, J.S., Kravtsov, A.V., Weinberg, D.H., (2001) ApJ, 548, p. 33; Carlberg, R.G., (2001) ApJ, 552, p. 427; Chiba, M., Beers, T.C., (2000) AJ, 119, p. 2843; Cooper, M.C., Newman, J.A., Yan, R., (2009) ApJ, 704, p. 687; Da Rocha, C., Mendes de Oliveira, C., (2005) MNRAS, 364, p. 1069; Da Rocha, C., Ziegler, B.L., Mendes de Oliveira, C., (2008) MNRAS, 388, p. 1433; Dilday, B., (2008) ApJ, 682, p. 262; Font, A.S., (2008) ApJ, 673, p. 215; Frieman, J.A., (2008) AJ, 135, p. 338; Gal-Yam, A., Maoz, D., Guhathakurta, P., Filippenko, A.V., (2003) AJ, 125, p. 1087; Gilbank, D.G., Balogh, M.L., (2008) MNRAS, 385, pp. L116; Gonzalez, A.H., Zaritsky, D., Zabludoff, A.I., (2007) ApJ, 666, p. 147; Graham, M.L., (2008) AJ, 135, p. 1343; Huchra, J.P., Geller, M.J., (1982) ApJ, 257, p. 423; Kauffmann, G., (2003) MNRAS, 341, p. 33; Law, D.R., Johnston, K.V., Majewski, S.R., (2005) ApJ, 619, p. 807; McGee, S.L., (2009) MNRAS, 400, p. 937; Mannucci, F., (2005) A&A, 433, p. 807; Milne, M.L., (2007) AJ, 133, p. 177; Purcell, C.W., Bullock, J.S., Zentner, A.R., (2007) ApJ, 666, p. 20; Sako, M., (2008) AJ, 135, p. 348; Sand, D.J., (2008) AJ, 135, p. 1917; Scannapieco, E., Bildsten, L., (2005) ApJ, 629, pp. L85; Scheick, X., Kuhn, J.R., (1994) ApJ, 423, p. 566; Searle, L., Zinn, R., (1978) ApJ, 225, p. 357; Spergel, D.N., (2007) ApJS, 170, p. 377; Sun, M., Donahue, M., Voit, G.M., (2007) ApJ, 671, p. 190; Sun, M., (2009) ApJ, 693, p. 1142; Sun, M., (2010) ApJ, 708, p. 946; Thuan, T.X., Kormendy, J., (1977) PASP, 89, p. 466; Vikhlinin, A., (2006) ApJ, 640, p. 691; Weinmann, S.M., (2006) MNRAS, 372, p. 1161; White, P.M., (2003) ApJ, 585, p. 739; Willman, B., Governato, F., Wadsley, J., Quinn, T., (2004) MNRAS, 355, p. 159; Yang, X., (2007) ApJ, 671, p. 153; Yang, X., Mo, H.J., van den Bosch, F.C., (2009) ApJ, 695, p. 900; Yanny, B., (2000) ApJ, 540, p. 825; Zheng, C., (2008) AJ, 135, p. 1766; Zibetti, S., White, S.D.M., Schneider, D.P., Brinkmann, J., (2005) MNRAS, 358, p. 949; Zwicky, F., (1951) PASP, 63, p. 61

Keywords

Galaxies: evolution
Galaxies: formation
Galaxies: structure

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10.1111/j.1745-3933.2010.00819.x

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@article{ad587dd9f9264b6d8f64fba84239a5ee,

title = "Constraints on intragroup stellar mass from hostless Type Ia supernovae",

abstract = "We probe the diffuse stellar mass in a sample of 1401 low-redshift galaxy groups (1013-1014 h-1 M⊙) by examining the rate of hostless Type Ia supernovae (SNe Ia) within the groups. We correlate the sample of confirmed SNe Ia from the Sloan Digital Sky Survey SN survey with the positions of our galaxy groups, as well as with the resolved galaxies within them. We find that 19 of the 59 SNe Ia within the group sample have no detectable host galaxy, with another three ambiguous instances. This gives a robust upper limit that a maximum of 2.69+1.58-1.34 per cent of the group's total mass arises from diffuse stars in the intragroup medium. After correcting for a contribution from 'prompt' SNe occurring within galaxies, and including a contribution from those which arise in dwarf galaxies below our photometric limit, we find that only 1.32+0.78-0.70 per cent of the group's total mass is likely in the form of diffuse stellar mass. Combining this result with the galaxy stellar mass functions of Yang, Mo and van den Bosch, we find that 47+16-15 per cent of the stellar mass in our groups is in the form of diffuse light, so that stars make up a fraction 0.028+0.011-0.010 of the total group mass. Galaxy groups appear to be very efficient in disrupting stellar mass into a diffuse component; however, stars still make up a small fraction of the group mass, comparable to that seen in rich clusters. This remains a challenge to galaxy formation models. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.",

keywords = "Galaxies: evolution, Galaxies: formation, Galaxies: structure",

author = "S.L. McGee and M.L. Balogh",

note = "Export Date: 15 August 2017 Correspondence Address: McGee, S.L.; Department of Physics and Astronomy, University of Waterloo, Waterloo, ON N2L 3G1, Canada; email: s2mcgee@uwaterloo.ca References: Balogh, M.L., McCarthy, I.G., Bower, R.G., Eke, V.R., (2008) MNRAS, 385, p. 1003; Bazin, G., (2009) A&A, 499, p. 653; Berlind, A.A., (2006) ApJS, 167, p. 1; Berrier, J.C., (2009) ApJ, 690, p. 1292; Blanton, M.R., (2003) ApJ, 592, p. 819; Brinchmann, J., (2004) MNRAS, 351, p. 1151; Bullock, J.S., Kravtsov, A.V., Weinberg, D.H., (2001) ApJ, 548, p. 33; Carlberg, R.G., (2001) ApJ, 552, p. 427; Chiba, M., Beers, T.C., (2000) AJ, 119, p. 2843; Cooper, M.C., Newman, J.A., Yan, R., (2009) ApJ, 704, p. 687; Da Rocha, C., Mendes de Oliveira, C., (2005) MNRAS, 364, p. 1069; Da Rocha, C., Ziegler, B.L., Mendes de Oliveira, C., (2008) MNRAS, 388, p. 1433; Dilday, B., (2008) ApJ, 682, p. 262; Font, A.S., (2008) ApJ, 673, p. 215; Frieman, J.A., (2008) AJ, 135, p. 338; Gal-Yam, A., Maoz, D., Guhathakurta, P., Filippenko, A.V., (2003) AJ, 125, p. 1087; Gilbank, D.G., Balogh, M.L., (2008) MNRAS, 385, pp. L116; Gonzalez, A.H., Zaritsky, D., Zabludoff, A.I., (2007) ApJ, 666, p. 147; Graham, M.L., (2008) AJ, 135, p. 1343; Huchra, J.P., Geller, M.J., (1982) ApJ, 257, p. 423; Kauffmann, G., (2003) MNRAS, 341, p. 33; Law, D.R., Johnston, K.V., Majewski, S.R., (2005) ApJ, 619, p. 807; McGee, S.L., (2009) MNRAS, 400, p. 937; Mannucci, F., (2005) A&A, 433, p. 807; Milne, M.L., (2007) AJ, 133, p. 177; Purcell, C.W., Bullock, J.S., Zentner, A.R., (2007) ApJ, 666, p. 20; Sako, M., (2008) AJ, 135, p. 348; Sand, D.J., (2008) AJ, 135, p. 1917; Scannapieco, E., Bildsten, L., (2005) ApJ, 629, pp. L85; Scheick, X., Kuhn, J.R., (1994) ApJ, 423, p. 566; Searle, L., Zinn, R., (1978) ApJ, 225, p. 357; Spergel, D.N., (2007) ApJS, 170, p. 377; Sun, M., Donahue, M., Voit, G.M., (2007) ApJ, 671, p. 190; Sun, M., (2009) ApJ, 693, p. 1142; Sun, M., (2010) ApJ, 708, p. 946; Thuan, T.X., Kormendy, J., (1977) PASP, 89, p. 466; Vikhlinin, A., (2006) ApJ, 640, p. 691; Weinmann, S.M., (2006) MNRAS, 372, p. 1161; White, P.M., (2003) ApJ, 585, p. 739; Willman, B., Governato, F., Wadsley, J., Quinn, T., (2004) MNRAS, 355, p. 159; Yang, X., (2007) ApJ, 671, p. 153; Yang, X., Mo, H.J., van den Bosch, F.C., (2009) ApJ, 695, p. 900; Yanny, B., (2000) ApJ, 540, p. 825; Zheng, C., (2008) AJ, 135, p. 1766; Zibetti, S., White, S.D.M., Schneider, D.P., Brinkmann, J., (2005) MNRAS, 358, p. 949; Zwicky, F., (1951) PASP, 63, p. 61",

year = "2010",

doi = "10.1111/j.1745-3933.2010.00819.x",

language = "English",

volume = "403",

pages = "L79--L83",

journal = "Monthly Notices of the Royal Astronomical Society: Letters",

issn = "17453933",

publisher = "Oxford University Press",

number = "1",

}

TY - JOUR

T1 - Constraints on intragroup stellar mass from hostless Type Ia supernovae

AU - McGee, S.L.

AU - Balogh, M.L.

N1 - Export Date: 15 August 2017 Correspondence Address: McGee, S.L.; Department of Physics and Astronomy, University of Waterloo, Waterloo, ON N2L 3G1, Canada; email: s2mcgee@uwaterloo.ca References: Balogh, M.L., McCarthy, I.G., Bower, R.G., Eke, V.R., (2008) MNRAS, 385, p. 1003; Bazin, G., (2009) A&A, 499, p. 653; Berlind, A.A., (2006) ApJS, 167, p. 1; Berrier, J.C., (2009) ApJ, 690, p. 1292; Blanton, M.R., (2003) ApJ, 592, p. 819; Brinchmann, J., (2004) MNRAS, 351, p. 1151; Bullock, J.S., Kravtsov, A.V., Weinberg, D.H., (2001) ApJ, 548, p. 33; Carlberg, R.G., (2001) ApJ, 552, p. 427; Chiba, M., Beers, T.C., (2000) AJ, 119, p. 2843; Cooper, M.C., Newman, J.A., Yan, R., (2009) ApJ, 704, p. 687; Da Rocha, C., Mendes de Oliveira, C., (2005) MNRAS, 364, p. 1069; Da Rocha, C., Ziegler, B.L., Mendes de Oliveira, C., (2008) MNRAS, 388, p. 1433; Dilday, B., (2008) ApJ, 682, p. 262; Font, A.S., (2008) ApJ, 673, p. 215; Frieman, J.A., (2008) AJ, 135, p. 338; Gal-Yam, A., Maoz, D., Guhathakurta, P., Filippenko, A.V., (2003) AJ, 125, p. 1087; Gilbank, D.G., Balogh, M.L., (2008) MNRAS, 385, pp. L116; Gonzalez, A.H., Zaritsky, D., Zabludoff, A.I., (2007) ApJ, 666, p. 147; Graham, M.L., (2008) AJ, 135, p. 1343; Huchra, J.P., Geller, M.J., (1982) ApJ, 257, p. 423; Kauffmann, G., (2003) MNRAS, 341, p. 33; Law, D.R., Johnston, K.V., Majewski, S.R., (2005) ApJ, 619, p. 807; McGee, S.L., (2009) MNRAS, 400, p. 937; Mannucci, F., (2005) A&A, 433, p. 807; Milne, M.L., (2007) AJ, 133, p. 177; Purcell, C.W., Bullock, J.S., Zentner, A.R., (2007) ApJ, 666, p. 20; Sako, M., (2008) AJ, 135, p. 348; Sand, D.J., (2008) AJ, 135, p. 1917; Scannapieco, E., Bildsten, L., (2005) ApJ, 629, pp. L85; Scheick, X., Kuhn, J.R., (1994) ApJ, 423, p. 566; Searle, L., Zinn, R., (1978) ApJ, 225, p. 357; Spergel, D.N., (2007) ApJS, 170, p. 377; Sun, M., Donahue, M., Voit, G.M., (2007) ApJ, 671, p. 190; Sun, M., (2009) ApJ, 693, p. 1142; Sun, M., (2010) ApJ, 708, p. 946; Thuan, T.X., Kormendy, J., (1977) PASP, 89, p. 466; Vikhlinin, A., (2006) ApJ, 640, p. 691; Weinmann, S.M., (2006) MNRAS, 372, p. 1161; White, P.M., (2003) ApJ, 585, p. 739; Willman, B., Governato, F., Wadsley, J., Quinn, T., (2004) MNRAS, 355, p. 159; Yang, X., (2007) ApJ, 671, p. 153; Yang, X., Mo, H.J., van den Bosch, F.C., (2009) ApJ, 695, p. 900; Yanny, B., (2000) ApJ, 540, p. 825; Zheng, C., (2008) AJ, 135, p. 1766; Zibetti, S., White, S.D.M., Schneider, D.P., Brinkmann, J., (2005) MNRAS, 358, p. 949; Zwicky, F., (1951) PASP, 63, p. 61

PY - 2010

Y1 - 2010

N2 - We probe the diffuse stellar mass in a sample of 1401 low-redshift galaxy groups (1013-1014 h-1 M⊙) by examining the rate of hostless Type Ia supernovae (SNe Ia) within the groups. We correlate the sample of confirmed SNe Ia from the Sloan Digital Sky Survey SN survey with the positions of our galaxy groups, as well as with the resolved galaxies within them. We find that 19 of the 59 SNe Ia within the group sample have no detectable host galaxy, with another three ambiguous instances. This gives a robust upper limit that a maximum of 2.69+1.58-1.34 per cent of the group's total mass arises from diffuse stars in the intragroup medium. After correcting for a contribution from 'prompt' SNe occurring within galaxies, and including a contribution from those which arise in dwarf galaxies below our photometric limit, we find that only 1.32+0.78-0.70 per cent of the group's total mass is likely in the form of diffuse stellar mass. Combining this result with the galaxy stellar mass functions of Yang, Mo and van den Bosch, we find that 47+16-15 per cent of the stellar mass in our groups is in the form of diffuse light, so that stars make up a fraction 0.028+0.011-0.010 of the total group mass. Galaxy groups appear to be very efficient in disrupting stellar mass into a diffuse component; however, stars still make up a small fraction of the group mass, comparable to that seen in rich clusters. This remains a challenge to galaxy formation models. © 2010 The Authors. Journal compilation © 2010 RAS.

AB - We probe the diffuse stellar mass in a sample of 1401 low-redshift galaxy groups (1013-1014 h-1 M⊙) by examining the rate of hostless Type Ia supernovae (SNe Ia) within the groups. We correlate the sample of confirmed SNe Ia from the Sloan Digital Sky Survey SN survey with the positions of our galaxy groups, as well as with the resolved galaxies within them. We find that 19 of the 59 SNe Ia within the group sample have no detectable host galaxy, with another three ambiguous instances. This gives a robust upper limit that a maximum of 2.69+1.58-1.34 per cent of the group's total mass arises from diffuse stars in the intragroup medium. After correcting for a contribution from 'prompt' SNe occurring within galaxies, and including a contribution from those which arise in dwarf galaxies below our photometric limit, we find that only 1.32+0.78-0.70 per cent of the group's total mass is likely in the form of diffuse stellar mass. Combining this result with the galaxy stellar mass functions of Yang, Mo and van den Bosch, we find that 47+16-15 per cent of the stellar mass in our groups is in the form of diffuse light, so that stars make up a fraction 0.028+0.011-0.010 of the total group mass. Galaxy groups appear to be very efficient in disrupting stellar mass into a diffuse component; however, stars still make up a small fraction of the group mass, comparable to that seen in rich clusters. This remains a challenge to galaxy formation models. © 2010 The Authors. Journal compilation © 2010 RAS.

KW - Galaxies: evolution

KW - Galaxies: formation

KW - Galaxies: structure

U2 - 10.1111/j.1745-3933.2010.00819.x

DO - 10.1111/j.1745-3933.2010.00819.x

M3 - Article

SN - 17453933

VL - 403

SP - L79-L83

JO - Monthly Notices of the Royal Astronomical Society: Letters

JF - Monthly Notices of the Royal Astronomical Society: Letters

IS - 1

ER -

Constraints on intragroup stellar mass from hostless Type Ia supernovae

Abstract

Bibliographical note

Keywords

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