From star-forming spirals to passive spheroids: Integral field spectroscopy of E+A galaxies

A.M. Swinbank; M.L. Balogh; R.G. Bower; A.I. Zabludoff; J.R. Lucey; S.L. Mcgee; C.J. Miller; R.C. Nichol

doi:10.1111/j.1365-2966.2011.20082.x

From star-forming spirals to passive spheroids: Integral field spectroscopy of E+A galaxies

A.M. Swinbank, M.L. Balogh, R.G. Bower, A.I. Zabludoff, J.R. Lucey, S.L. Mcgee, C.J. Miller, R.C. Nichol

Physics and Astronomy

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

27 Citations (Scopus)

Abstract

We present three-dimensional spectroscopy of 11 E+A galaxies at z= 0.06-0.12. These galaxies were selected for their strong Hδ absorption but weak (or non-existent) [Oii] λ3727 and Hα emission. This selection suggests that a recent burst of star formation was triggered but subsequently abruptly ended. We probe the spatial and spectral properties of both the young (≲1Gyr) and old (≳few Gyr) stellar populations. Using the Hδ equivalent widths we estimate that the burst masses must have been at least 10 per cent by mass (M burst≳ 10 10M ⊙), which is also consistent with the star formation history inferred from the broad-band spectral energy distributions. On average the A stars cover ∼33 per cent of the galaxy image, extending over 2-15kpc 2, indicating that the characteristic E+A signature is a property of the galaxy as a whole and not due to a heterogeneous mixture of populations. In approximately half of the sample, we find that the A stars, nebular emission and continuum emission are not co-located, suggesting that the newest stars are forming in a different place than those that formed ≲1Gyr ago, and that recent star formation has occurred in regions distinct from the oldest stellar populations. At least 10 of the galaxies (91 per cent) have dynamics that class them as 'fast rotators' with magnitudes, v/σ, λ R and bulge-to-total (B/T) ratio comparable to local, representative ellipticals and S0s. We also find a correlation between the spatial extent of the A stars and the dynamical state of the galaxy such that the fastest rotators tend to have the most compact A star populations, providing new constraints on models that aim to explain the transformation of later type galaxies into early types. Finally, we show that there are no obvious differences between the line extents and kinematics of E+A galaxies detected in the radio (active galactic nucleus, AGN) compared to non-radio sources, suggesting that AGN feedback does not play a dramatic role in defining their properties, and/or that its effects are short. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.

Original language	English
Pages (from-to)	672-683
Number of pages	12
Journal	Royal Astronomical Society. Monthly Notices
Volume	420
Issue number	1
DOIs	https://doi.org/10.1111/j.1365-2966.2011.20082.x
Publication status	Published - 2012

Bibliographical note

Export Date: 15 August 2017

CODEN: MNRAA

Correspondence Address: Swinbank, A.M.; Institute for Computational Cosmology, Department of Physics and Astronomy, University of Durham, South Road, Durham DH1 3LE, United Kingdom; email: a.m.swinbank@dur.ac.uk

References: Allington-Smith, J., (2002) PASP, 114, p. 892; Balcells, M., Peletier, R.F., (1994) AJ, 107, p. 135; Balogh, M.L., Morris, S.L., Yee, H.K.C., Carlberg, R.G., Ellingson, E., (1999) ApJ, 527, p. 54; Balogh, M.L., Miller, C., Nichol, R., Zabludoff, A., Goto, T., (2005) MNRAS, 360, p. 587; Balogh, M.L., (2009) MNRAS, 398, p. 754; Bekki, K., Couch, W.J., Shioya, Y., Vazdekis, A., (2005) MNRAS, 359, p. 949; Bender, R., Burstein, D., Faber, S.M., (1992) ApJ, 399, p. 462; Bender, R., Saglia, R.P., Gerhard, O.E., (1994) MNRAS, 269, p. 785; Bernardi, M., Sheth, R.K., Nichol, R.C., Schneider, D.P., Brinkmann, J., (2005) AJ, 129, p. 61; Bertelli, G., Bressan, A., Chiosi, C., Fagotto, F., Nasi, E., (1994) A&AS, 106, p. 275; Bower, R.G., Benson, A.J., Malbon, R., Helly, J.C., Frenk, C.S., Baugh, C.M., Cole, S., Lacey, C.G., (2006) MNRAS, 370, p. 645; Bruzual, G., Charlot, S., (2003) MNRAS, 344, p. 1000; Cappellari, M., Copin, Y., (2003) MNRAS, 342, p. 345; Cappellari, M., Emsellem, E., (2004) PASP, 116, p. 138; Couch, W.J., Sharples, R.M., (1987) MNRAS, 229, p. 423; Courteau, S., (1997) AJ, 114, p. 2402; Dressler, A., Gunn, J.E., (1982) ApJ, 263, p. 533; Dressler, A., Gunn, J.E., (1983) ApJ, 270, p. 7; Emsellem, E., (2007) MNRAS, 379, p. 401; Faber, S.M., Jackson, R.E., (1976) ApJ, 204, p. 668; Faber, S.M., (1997) AJ, 114, p. 1771; Georgakakis, A., (2008) MNRAS, 385, p. 2049; Goto, T., (2003) PASJ, 55, p. 771; Goto, T., Kawai, A., Shimono, A., Sugai, H., Yagi, M., Hattori, T., (2008) MNRAS, 386, p. 1355; Helou, G., Soifer, B.T., Rowan-Robinson, M., (1985) ApJ, 298, pp. L7; Jacoby, G.H., Hunter, D.A., Christian, C.A., (1984) ApJS, 56, p. 257; Kennicutt, R.C., (1998) ARA&A, 36, p. 189; Kormendy, J., Djorgovski, S., (1989) ARA&A, 27, p. 235; McGee, S.L., Balogh, M.L., Wilman, D.J., Bower, R.G., Mulchaey, J.S., Parker, L.C., Oemler, A., (2011) MNRAS, 413, p. 996; Maraston, C., (1998) MNRAS, 300, p. 872; Mihos, J.C., Hernquist, L., (1996) ApJ, 464, p. 641; Miller, C.J., (2005) AJ, 130, p. 968; Naab, T., Burkert, A., (2003) ApJ, 597, p. 893; Naab, T., Burkert, A., Hernquist, L., (1999) ApJ, 523, pp. L133; Norton, S.A., Gebhardt, K., Zabludoff, A.I., Zaritsky, D., (2001) ApJ, 557, p. 150; Poggianti, B.M., Smail, I., Dressler, A., Couch, W.J., Barger, A.J., Butcher, H., Ellis, R.S., Oemler, A.J., (1999) ApJ, 518, p. 576; Pracy, M.B., Couch, W.J., Blake, C., Bekki, K., Harrison, C., Colless, M., Kuntschner, H., de Propris, R., (2005) MNRAS, 359, p. 1421; Pracy, M.B., Kuntschner, H., Couch, W.J., Blake, C., Bekki, K., Briggs, F., (2009) MNRAS, 396, p. 1349; Pracy, M.B., Couch, W.J., Kuntschner, H., (2010) Publ. Astron. Soc. Australia, 27, p. 360; Rose, J.A., (1985) AJ, 90, p. 1927; Salim, S., (2007) ApJS, 173, p. 267; Salpeter, E.E., (1955) ApJ, 121, p. 161; Shioya, Y., Bekki, K., Couch, W.J., (2004) ApJ, 601, p. 654; Swinbank, A.M., Balogh, M.L., Bower, R.G., Hau, G.K.T., Allington-Smith, J.R., Nichol, R.C., Miller, C.J., (2005) ApJ, 622, p. 260; Tran, K.-V.H., Franx, M., Illingworth, G., Kelson, D.D., van Dokkum, P., (2003) ApJ, 599, p. 865; Tran, K.-V.H., Franx, M., Illingworth, G.D., van Dokkum, P., Kelson, D.D., Magee, D., (2004) ApJ, 609, p. 683; Tremonti, C.A., Moustakas, J., Diamond-Stanic, A.M., (2007) ApJ, 663, pp. L77; Vazdekis, A., Arimoto, N., (1999) ApJ, 525, p. 144; Wolf, C., Gray, M.E., Meisenheimer, K., (2005) A&A, 443, p. 435; Yamauchi, C., Goto, T., (2005) MNRAS, 359, p. 1557; Yan, R., Newman, J.A., Faber, S.M., Konidaris, N., Koo, D., Davis, M., (2006) ApJ, 648, p. 281; Yan, R., (2009) MNRAS, 398, p. 735; Yang, Y., Zabludoff, A.I., Zaritsky, D., Lauer, T.R., Mihos, J.C., (2004) ApJ, 607, p. 258; Yang, Y., Zabludoff, A.I., Zaritsky, D., Mihos, J.C., (2008) ApJ, 688, p. 945; Zabludoff, A.I., Zaritsky, D., Lin, H., Tucker, D., Hashimoto, Y., Shectman, S.A., Oemler, A., Kirshner, R.P., (1996) ApJ, 466, p. 104

Keywords

Galaxies: evolution
Galaxies: kinematics and dynamics
Galaxies: starburst
Galaxies: stellar content

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10.1111/j.1365-2966.2011.20082.x

https://www.scopus.com/inward/record.uri?eid=2-s2.0-84856217916&doi=10.1111%2fj.1365-2966.2011.20082.x&partnerID=40&md5=d67eea36663c3cea28ba77a1b7b765f6

Cite this

@article{bff0d7f30b5949a795c0b4208353100b,

title = "From star-forming spirals to passive spheroids: Integral field spectroscopy of E+A galaxies",

abstract = "We present three-dimensional spectroscopy of 11 E+A galaxies at z= 0.06-0.12. These galaxies were selected for their strong Hδ absorption but weak (or non-existent) [Oii] λ3727 and Hα emission. This selection suggests that a recent burst of star formation was triggered but subsequently abruptly ended. We probe the spatial and spectral properties of both the young (≲1Gyr) and old (≳few Gyr) stellar populations. Using the Hδ equivalent widths we estimate that the burst masses must have been at least 10 per cent by mass (M burst≳ 10 10M ⊙), which is also consistent with the star formation history inferred from the broad-band spectral energy distributions. On average the A stars cover ∼33 per cent of the galaxy image, extending over 2-15kpc 2, indicating that the characteristic E+A signature is a property of the galaxy as a whole and not due to a heterogeneous mixture of populations. In approximately half of the sample, we find that the A stars, nebular emission and continuum emission are not co-located, suggesting that the newest stars are forming in a different place than those that formed ≲1Gyr ago, and that recent star formation has occurred in regions distinct from the oldest stellar populations. At least 10 of the galaxies (91 per cent) have dynamics that class them as 'fast rotators' with magnitudes, v/σ, λ R and bulge-to-total (B/T) ratio comparable to local, representative ellipticals and S0s. We also find a correlation between the spatial extent of the A stars and the dynamical state of the galaxy such that the fastest rotators tend to have the most compact A star populations, providing new constraints on models that aim to explain the transformation of later type galaxies into early types. Finally, we show that there are no obvious differences between the line extents and kinematics of E+A galaxies detected in the radio (active galactic nucleus, AGN) compared to non-radio sources, suggesting that AGN feedback does not play a dramatic role in defining their properties, and/or that its effects are short. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.",

keywords = "Galaxies: evolution, Galaxies: kinematics and dynamics, Galaxies: starburst, Galaxies: stellar content",

author = "A.M. Swinbank and M.L. Balogh and R.G. Bower and A.I. Zabludoff and J.R. Lucey and S.L. Mcgee and C.J. Miller and R.C. Nichol",

note = "Export Date: 15 August 2017 CODEN: MNRAA Correspondence Address: Swinbank, A.M.; Institute for Computational Cosmology, Department of Physics and Astronomy, University of Durham, South Road, Durham DH1 3LE, United Kingdom; email: a.m.swinbank@dur.ac.uk References: Allington-Smith, J., (2002) PASP, 114, p. 892; Balcells, M., Peletier, R.F., (1994) AJ, 107, p. 135; Balogh, M.L., Morris, S.L., Yee, H.K.C., Carlberg, R.G., Ellingson, E., (1999) ApJ, 527, p. 54; Balogh, M.L., Miller, C., Nichol, R., Zabludoff, A., Goto, T., (2005) MNRAS, 360, p. 587; Balogh, M.L., (2009) MNRAS, 398, p. 754; Bekki, K., Couch, W.J., Shioya, Y., Vazdekis, A., (2005) MNRAS, 359, p. 949; Bender, R., Burstein, D., Faber, S.M., (1992) ApJ, 399, p. 462; Bender, R., Saglia, R.P., Gerhard, O.E., (1994) MNRAS, 269, p. 785; Bernardi, M., Sheth, R.K., Nichol, R.C., Schneider, D.P., Brinkmann, J., (2005) AJ, 129, p. 61; Bertelli, G., Bressan, A., Chiosi, C., Fagotto, F., Nasi, E., (1994) A&AS, 106, p. 275; Bower, R.G., Benson, A.J., Malbon, R., Helly, J.C., Frenk, C.S., Baugh, C.M., Cole, S., Lacey, C.G., (2006) MNRAS, 370, p. 645; Bruzual, G., Charlot, S., (2003) MNRAS, 344, p. 1000; Cappellari, M., Copin, Y., (2003) MNRAS, 342, p. 345; Cappellari, M., Emsellem, E., (2004) PASP, 116, p. 138; Couch, W.J., Sharples, R.M., (1987) MNRAS, 229, p. 423; Courteau, S., (1997) AJ, 114, p. 2402; Dressler, A., Gunn, J.E., (1982) ApJ, 263, p. 533; Dressler, A., Gunn, J.E., (1983) ApJ, 270, p. 7; Emsellem, E., (2007) MNRAS, 379, p. 401; Faber, S.M., Jackson, R.E., (1976) ApJ, 204, p. 668; Faber, S.M., (1997) AJ, 114, p. 1771; Georgakakis, A., (2008) MNRAS, 385, p. 2049; Goto, T., (2003) PASJ, 55, p. 771; Goto, T., Kawai, A., Shimono, A., Sugai, H., Yagi, M., Hattori, T., (2008) MNRAS, 386, p. 1355; Helou, G., Soifer, B.T., Rowan-Robinson, M., (1985) ApJ, 298, pp. L7; Jacoby, G.H., Hunter, D.A., Christian, C.A., (1984) ApJS, 56, p. 257; Kennicutt, R.C., (1998) ARA&A, 36, p. 189; Kormendy, J., Djorgovski, S., (1989) ARA&A, 27, p. 235; McGee, S.L., Balogh, M.L., Wilman, D.J., Bower, R.G., Mulchaey, J.S., Parker, L.C., Oemler, A., (2011) MNRAS, 413, p. 996; Maraston, C., (1998) MNRAS, 300, p. 872; Mihos, J.C., Hernquist, L., (1996) ApJ, 464, p. 641; Miller, C.J., (2005) AJ, 130, p. 968; Naab, T., Burkert, A., (2003) ApJ, 597, p. 893; Naab, T., Burkert, A., Hernquist, L., (1999) ApJ, 523, pp. L133; Norton, S.A., Gebhardt, K., Zabludoff, A.I., Zaritsky, D., (2001) ApJ, 557, p. 150; Poggianti, B.M., Smail, I., Dressler, A., Couch, W.J., Barger, A.J., Butcher, H., Ellis, R.S., Oemler, A.J., (1999) ApJ, 518, p. 576; Pracy, M.B., Couch, W.J., Blake, C., Bekki, K., Harrison, C., Colless, M., Kuntschner, H., de Propris, R., (2005) MNRAS, 359, p. 1421; Pracy, M.B., Kuntschner, H., Couch, W.J., Blake, C., Bekki, K., Briggs, F., (2009) MNRAS, 396, p. 1349; Pracy, M.B., Couch, W.J., Kuntschner, H., (2010) Publ. Astron. Soc. Australia, 27, p. 360; Rose, J.A., (1985) AJ, 90, p. 1927; Salim, S., (2007) ApJS, 173, p. 267; Salpeter, E.E., (1955) ApJ, 121, p. 161; Shioya, Y., Bekki, K., Couch, W.J., (2004) ApJ, 601, p. 654; Swinbank, A.M., Balogh, M.L., Bower, R.G., Hau, G.K.T., Allington-Smith, J.R., Nichol, R.C., Miller, C.J., (2005) ApJ, 622, p. 260; Tran, K.-V.H., Franx, M., Illingworth, G., Kelson, D.D., van Dokkum, P., (2003) ApJ, 599, p. 865; Tran, K.-V.H., Franx, M., Illingworth, G.D., van Dokkum, P., Kelson, D.D., Magee, D., (2004) ApJ, 609, p. 683; Tremonti, C.A., Moustakas, J., Diamond-Stanic, A.M., (2007) ApJ, 663, pp. L77; Vazdekis, A., Arimoto, N., (1999) ApJ, 525, p. 144; Wolf, C., Gray, M.E., Meisenheimer, K., (2005) A&A, 443, p. 435; Yamauchi, C., Goto, T., (2005) MNRAS, 359, p. 1557; Yan, R., Newman, J.A., Faber, S.M., Konidaris, N., Koo, D., Davis, M., (2006) ApJ, 648, p. 281; Yan, R., (2009) MNRAS, 398, p. 735; Yang, Y., Zabludoff, A.I., Zaritsky, D., Lauer, T.R., Mihos, J.C., (2004) ApJ, 607, p. 258; Yang, Y., Zabludoff, A.I., Zaritsky, D., Mihos, J.C., (2008) ApJ, 688, p. 945; Zabludoff, A.I., Zaritsky, D., Lin, H., Tucker, D., Hashimoto, Y., Shectman, S.A., Oemler, A., Kirshner, R.P., (1996) ApJ, 466, p. 104",

year = "2012",

doi = "10.1111/j.1365-2966.2011.20082.x",

language = "English",

volume = "420",

pages = "672--683",

journal = "Royal Astronomical Society. Monthly Notices",

issn = "0035-8711",

publisher = "SIPRI/Oxford University Press",

number = "1",

}

TY - JOUR

T1 - From star-forming spirals to passive spheroids: Integral field spectroscopy of E+A galaxies

AU - Swinbank, A.M.

AU - Balogh, M.L.

AU - Bower, R.G.

AU - Zabludoff, A.I.

AU - Lucey, J.R.

AU - Mcgee, S.L.

AU - Miller, C.J.

AU - Nichol, R.C.

N1 - Export Date: 15 August 2017 CODEN: MNRAA Correspondence Address: Swinbank, A.M.; Institute for Computational Cosmology, Department of Physics and Astronomy, University of Durham, South Road, Durham DH1 3LE, United Kingdom; email: a.m.swinbank@dur.ac.uk References: Allington-Smith, J., (2002) PASP, 114, p. 892; Balcells, M., Peletier, R.F., (1994) AJ, 107, p. 135; Balogh, M.L., Morris, S.L., Yee, H.K.C., Carlberg, R.G., Ellingson, E., (1999) ApJ, 527, p. 54; Balogh, M.L., Miller, C., Nichol, R., Zabludoff, A., Goto, T., (2005) MNRAS, 360, p. 587; Balogh, M.L., (2009) MNRAS, 398, p. 754; Bekki, K., Couch, W.J., Shioya, Y., Vazdekis, A., (2005) MNRAS, 359, p. 949; Bender, R., Burstein, D., Faber, S.M., (1992) ApJ, 399, p. 462; Bender, R., Saglia, R.P., Gerhard, O.E., (1994) MNRAS, 269, p. 785; Bernardi, M., Sheth, R.K., Nichol, R.C., Schneider, D.P., Brinkmann, J., (2005) AJ, 129, p. 61; Bertelli, G., Bressan, A., Chiosi, C., Fagotto, F., Nasi, E., (1994) A&AS, 106, p. 275; Bower, R.G., Benson, A.J., Malbon, R., Helly, J.C., Frenk, C.S., Baugh, C.M., Cole, S., Lacey, C.G., (2006) MNRAS, 370, p. 645; Bruzual, G., Charlot, S., (2003) MNRAS, 344, p. 1000; Cappellari, M., Copin, Y., (2003) MNRAS, 342, p. 345; Cappellari, M., Emsellem, E., (2004) PASP, 116, p. 138; Couch, W.J., Sharples, R.M., (1987) MNRAS, 229, p. 423; Courteau, S., (1997) AJ, 114, p. 2402; Dressler, A., Gunn, J.E., (1982) ApJ, 263, p. 533; Dressler, A., Gunn, J.E., (1983) ApJ, 270, p. 7; Emsellem, E., (2007) MNRAS, 379, p. 401; Faber, S.M., Jackson, R.E., (1976) ApJ, 204, p. 668; Faber, S.M., (1997) AJ, 114, p. 1771; Georgakakis, A., (2008) MNRAS, 385, p. 2049; Goto, T., (2003) PASJ, 55, p. 771; Goto, T., Kawai, A., Shimono, A., Sugai, H., Yagi, M., Hattori, T., (2008) MNRAS, 386, p. 1355; Helou, G., Soifer, B.T., Rowan-Robinson, M., (1985) ApJ, 298, pp. L7; Jacoby, G.H., Hunter, D.A., Christian, C.A., (1984) ApJS, 56, p. 257; Kennicutt, R.C., (1998) ARA&A, 36, p. 189; Kormendy, J., Djorgovski, S., (1989) ARA&A, 27, p. 235; McGee, S.L., Balogh, M.L., Wilman, D.J., Bower, R.G., Mulchaey, J.S., Parker, L.C., Oemler, A., (2011) MNRAS, 413, p. 996; Maraston, C., (1998) MNRAS, 300, p. 872; Mihos, J.C., Hernquist, L., (1996) ApJ, 464, p. 641; Miller, C.J., (2005) AJ, 130, p. 968; Naab, T., Burkert, A., (2003) ApJ, 597, p. 893; Naab, T., Burkert, A., Hernquist, L., (1999) ApJ, 523, pp. L133; Norton, S.A., Gebhardt, K., Zabludoff, A.I., Zaritsky, D., (2001) ApJ, 557, p. 150; Poggianti, B.M., Smail, I., Dressler, A., Couch, W.J., Barger, A.J., Butcher, H., Ellis, R.S., Oemler, A.J., (1999) ApJ, 518, p. 576; Pracy, M.B., Couch, W.J., Blake, C., Bekki, K., Harrison, C., Colless, M., Kuntschner, H., de Propris, R., (2005) MNRAS, 359, p. 1421; Pracy, M.B., Kuntschner, H., Couch, W.J., Blake, C., Bekki, K., Briggs, F., (2009) MNRAS, 396, p. 1349; Pracy, M.B., Couch, W.J., Kuntschner, H., (2010) Publ. Astron. Soc. Australia, 27, p. 360; Rose, J.A., (1985) AJ, 90, p. 1927; Salim, S., (2007) ApJS, 173, p. 267; Salpeter, E.E., (1955) ApJ, 121, p. 161; Shioya, Y., Bekki, K., Couch, W.J., (2004) ApJ, 601, p. 654; Swinbank, A.M., Balogh, M.L., Bower, R.G., Hau, G.K.T., Allington-Smith, J.R., Nichol, R.C., Miller, C.J., (2005) ApJ, 622, p. 260; Tran, K.-V.H., Franx, M., Illingworth, G., Kelson, D.D., van Dokkum, P., (2003) ApJ, 599, p. 865; Tran, K.-V.H., Franx, M., Illingworth, G.D., van Dokkum, P., Kelson, D.D., Magee, D., (2004) ApJ, 609, p. 683; Tremonti, C.A., Moustakas, J., Diamond-Stanic, A.M., (2007) ApJ, 663, pp. L77; Vazdekis, A., Arimoto, N., (1999) ApJ, 525, p. 144; Wolf, C., Gray, M.E., Meisenheimer, K., (2005) A&A, 443, p. 435; Yamauchi, C., Goto, T., (2005) MNRAS, 359, p. 1557; Yan, R., Newman, J.A., Faber, S.M., Konidaris, N., Koo, D., Davis, M., (2006) ApJ, 648, p. 281; Yan, R., (2009) MNRAS, 398, p. 735; Yang, Y., Zabludoff, A.I., Zaritsky, D., Lauer, T.R., Mihos, J.C., (2004) ApJ, 607, p. 258; Yang, Y., Zabludoff, A.I., Zaritsky, D., Mihos, J.C., (2008) ApJ, 688, p. 945; Zabludoff, A.I., Zaritsky, D., Lin, H., Tucker, D., Hashimoto, Y., Shectman, S.A., Oemler, A., Kirshner, R.P., (1996) ApJ, 466, p. 104

PY - 2012

Y1 - 2012

N2 - We present three-dimensional spectroscopy of 11 E+A galaxies at z= 0.06-0.12. These galaxies were selected for their strong Hδ absorption but weak (or non-existent) [Oii] λ3727 and Hα emission. This selection suggests that a recent burst of star formation was triggered but subsequently abruptly ended. We probe the spatial and spectral properties of both the young (≲1Gyr) and old (≳few Gyr) stellar populations. Using the Hδ equivalent widths we estimate that the burst masses must have been at least 10 per cent by mass (M burst≳ 10 10M ⊙), which is also consistent with the star formation history inferred from the broad-band spectral energy distributions. On average the A stars cover ∼33 per cent of the galaxy image, extending over 2-15kpc 2, indicating that the characteristic E+A signature is a property of the galaxy as a whole and not due to a heterogeneous mixture of populations. In approximately half of the sample, we find that the A stars, nebular emission and continuum emission are not co-located, suggesting that the newest stars are forming in a different place than those that formed ≲1Gyr ago, and that recent star formation has occurred in regions distinct from the oldest stellar populations. At least 10 of the galaxies (91 per cent) have dynamics that class them as 'fast rotators' with magnitudes, v/σ, λ R and bulge-to-total (B/T) ratio comparable to local, representative ellipticals and S0s. We also find a correlation between the spatial extent of the A stars and the dynamical state of the galaxy such that the fastest rotators tend to have the most compact A star populations, providing new constraints on models that aim to explain the transformation of later type galaxies into early types. Finally, we show that there are no obvious differences between the line extents and kinematics of E+A galaxies detected in the radio (active galactic nucleus, AGN) compared to non-radio sources, suggesting that AGN feedback does not play a dramatic role in defining their properties, and/or that its effects are short. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.

AB - We present three-dimensional spectroscopy of 11 E+A galaxies at z= 0.06-0.12. These galaxies were selected for their strong Hδ absorption but weak (or non-existent) [Oii] λ3727 and Hα emission. This selection suggests that a recent burst of star formation was triggered but subsequently abruptly ended. We probe the spatial and spectral properties of both the young (≲1Gyr) and old (≳few Gyr) stellar populations. Using the Hδ equivalent widths we estimate that the burst masses must have been at least 10 per cent by mass (M burst≳ 10 10M ⊙), which is also consistent with the star formation history inferred from the broad-band spectral energy distributions. On average the A stars cover ∼33 per cent of the galaxy image, extending over 2-15kpc 2, indicating that the characteristic E+A signature is a property of the galaxy as a whole and not due to a heterogeneous mixture of populations. In approximately half of the sample, we find that the A stars, nebular emission and continuum emission are not co-located, suggesting that the newest stars are forming in a different place than those that formed ≲1Gyr ago, and that recent star formation has occurred in regions distinct from the oldest stellar populations. At least 10 of the galaxies (91 per cent) have dynamics that class them as 'fast rotators' with magnitudes, v/σ, λ R and bulge-to-total (B/T) ratio comparable to local, representative ellipticals and S0s. We also find a correlation between the spatial extent of the A stars and the dynamical state of the galaxy such that the fastest rotators tend to have the most compact A star populations, providing new constraints on models that aim to explain the transformation of later type galaxies into early types. Finally, we show that there are no obvious differences between the line extents and kinematics of E+A galaxies detected in the radio (active galactic nucleus, AGN) compared to non-radio sources, suggesting that AGN feedback does not play a dramatic role in defining their properties, and/or that its effects are short. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.

KW - Galaxies: evolution

KW - Galaxies: kinematics and dynamics

KW - Galaxies: starburst

KW - Galaxies: stellar content

U2 - 10.1111/j.1365-2966.2011.20082.x

DO - 10.1111/j.1365-2966.2011.20082.x

M3 - Article

SN - 0035-8711

VL - 420

SP - 672

EP - 683

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

IS - 1

ER -

From star-forming spirals to passive spheroids: Integral field spectroscopy of E+A galaxies

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