Musical taste, in-group favouritism and social identity theory: Re-testing the predictions of the self-esteem hypothesis

Musical taste is thought to function as a social ‘badge’ of group membership, contributing to an individual’s sense of social identity. Following from this, social identity theory predicts that individuals should perceive those who share their musical tastes more favourably than those who do not. Social identity theory also asserts that this in-group favouritism is motivated by the need to achieve, maintain or enhance a positive social identity and self-esteem (i.e., the ‘self-esteem hypothesis’). The findings of the present study supported both of these predictions. Participants rated fans of their favourite musical style significantly more favourably than fans of their least favourite musical style. The present findings also offer, for the first time, evidence of significant positive correlations between an individual’s self-esteem and the in-group bias shown to those who share their musical tastes. However, significant relationships with in-group identification also indicate that self-esteem is unlikely to be the sole factor responsible for this apparent in-group bias. Together these findings suggest that those who share our musical taste are likely to be regarded as in-group members and will be subject to in-group favouritism according to our self-esteem and how strongly we identify with our fellow music fans.

Are the psychological benefits of choral singing unique to choirs? A comparison of six activity groups

The present study compared the psychological well-being of choral singers to those who took part in five other activities: solo singers, band / orchestra members, solo musicians, team sport players and solo sport players. These comparison groups were chosen because they each share (or lack) three key features of choral singing: (1) singing; (2) the production of music; and (3) membership of a social group or team. 194 participants completed an online questionnaire to assess their well-being and the extent to which their chosen activity satisfies their psychological needs for autonomy, competence and relatedness. Analysis indicated that participants who sang in a choir reported similar levels of psychological well-being, happiness, anxiety, depression and self-esteem to those who took part in the other five leisure activities. Significant differences were found on measures of autonomy and relatedness, but participants in all six groups also reported experiencing similar levels of competence when engaged in their chosen leisure activity. These findings suggest choral singing may not be uniquely beneficial and any leisure activity that offers opportunities for improvement, mastery of a new skill or a sense of accomplishment might have a positive effect on our psychological well-being

Emotional intelligence, alexithymia, stress and peoples’ reasons for listening to music

The present study investigated the relationship between people’s reasons for listening to music, trait emotional intelligence and alexithymia whilst also controlling for the effect of participants’ gender, age and perceived stress levels. In keeping with previous research, initial findings indicated that emotionally intelligent individuals were less likely to use music to relieve and alleviate negative moods, whilst those who had high scores on a measure of alexithymia were more likely to use music for the same reasons. However, when the effects of gender, age and perceived stress were controlled for these relationships were no longer significant and previously non-significant relationships between trait emotional intelligence and using music to manipulate arousal and to reminisce about the past were found to be significant. Together these findings suggest that emotional intelligence is related to the reasons why people listen to music but not in the way that previous research had suggested, and the apparent links between emotional intelligence and mood management might be might be better explained by the stress experienced by participants at the time of questioning

Self-to-stereotype matching and musical taste: Is there a link between self-to-stereotype similarity and self-rated music-genre preferences?

Musical taste is believed to function as a social ‘badge’ of identity that might develop according to a process of ‘self-to-stereotype matching’. For this reason, individuals were expected to like musical styles that are stereotypically associated with fans that were similar to them. Three studies, each using a different measure of self-to-stereotype similarity, found that similarity to stereotypical music fans correlated significantly with participants’ self-rated musical tastes. These findings suggested individuals were more likely to prefer a musical style if they were similar, or at least perceived themselves similar, to the stereotypical fans associated with that musical style. In all three studies, evidence was also found to suggest that an individual’s similarity to stereotypical music fans might be used to predict their favourite musical style

Submillimeter Follow-up of WISE-Selected Hyperluminous Galaxies

We have used the Caltech Submillimeter Observatory (CSO) to follow-up a sample of WISE-selected, hyperluminous galaxies, so called W1W2-dropout galaxies. This is a rare (~ 1000 all-sky) population of galaxies at high redshift (peaks at z=2-3), that are faint or undetected by WISE at 3.4 and 4.6 um, yet are clearly detected at 12 and 22 um. The optical spectra of most of these galaxies show significant AGN activity. We observed 14 high-redshift (z > 1.7) W1W2-dropout galaxies with SHARC-II at 350 to 850 um, with 9 detections; and observed 18 with Bolocam at 1.1 mm, with five detections. Warm Spitzer follow-up of 25 targets at 3.6 and 4.5 um, as well as optical spectra of 12 targets are also presented in the paper. Combining WISE data with observations from warm Spitzer and CSO, we constructed their mid-IR to millimeter spectral energy distributions (SEDs). These SEDs have a consistent shape, showing significantly higher mid-IR to submm ratios than other galaxy templates, suggesting a hotter dust temperature. We estimate their dust temperatures to be 60-120 K using a single-temperature model. Their infrared luminosities are well over 10^{13} Lsun. These SEDs are not well fitted with existing galaxy templates, suggesting they are a new population with very high luminosity and hot dust. They are likely among the most luminous galaxies in the Universe. We argue that they are extreme cases of luminous, hot dust-obscured galaxies (DOGs), possibly representing a short evolutionary phase during galaxy merging and evolution. A better understanding of their long-wavelength properties needs ALMA as well as Herschel data.Comment: Will be Published on Sep 1, 2012 by Ap

Observations of Arp 220 using Herschel-SPIRE: An Unprecedented View of the Molecular Gas in an Extreme Star Formation Environment

We present Herschel SPIRE-FTS observations of Arp~220, a nearby ULIRG. The FTS continuously covers 190 -- 670 microns, providing a good measurement of the continuum and detection of several molecular and atomic species. We detect luminous CO (J = 4-3 to 13-12) and water ladders with comparable total luminosity; very high-J HCN absorption; OH+, H2O+, and HF in absorption; and CI and NII. Modeling of the continuum yields warm dust, with T = 66 K, and an unusually large optical depth of ~5 at 100 microns. Non-LTE modeling of the CO shows two temperature components: cold molecular gas at T ~ 50 K and warm molecular gas at T ~1350 K. The mass of the warm gas is 10% of the cold gas, but dominates the luminosity of the CO ladder. The temperature of the warm gas is in excellent agreement with H2 rotational lines. At 1350 K, H2 dominates the cooling (~20 L_sun/M_sun) in the ISM compared to CO (~0.4 L_sun/M_sun). We found that only a non-ionizing source such as the mechanical energy from supernovae and stellar winds can excite the warm gas and satisfy the energy budget of ~20 L_sun/M_sun. We detect a massive molecular outflow in Arp 220 from the analysis of strong P-Cygni line profiles observed in OH+, H2O+, and H2O. The outflow has a mass > 10^{7} M_sun and is bound to the nuclei with velocity < 250 km/s. The large column densities observed for these molecular ions strongly favor the existence of an X-ray luminous AGN (10^{44} ergs/s) in Arp 220.Comment: Accepted in ApJ on September 1, 201

Submillimeter Follow-up of Wise-Selected Hyperluminous Galaxies

We have used the Caltech Submillimeter Observatory (CSO) to follow-up a sample of Wide-field Infrared Survey Explorer (WISE) selected, hyperluminous galaxies, the so-called W1W2-dropout galaxies. This is a rare (approximately 1000 all-sky) population of galaxies at high redshift (peaks at zeta = 2-3), which are faint or undetected by WISE at 3.4 and 4.6 micrometers, yet are clearly detected at 12 and 22 micrometers. The optical spectra of most of these galaxies show significant active galactic nucleus activity. We observed 14 high-redshift (zeta greater than 1.7) W1W2-dropout galaxies with SHARC-II at 350-850 micrometers, with nine detections, and observed 18 with Bolocam at 1.1 mm, with five detections. Warm Spitzer follow-up of 25 targets at 3.6 and 4.5 micrometers, as well as optical spectra of 12 targets, are also presented in the paper. Combining WISE data with observations from warm Spitzer and CSO, we constructed their mid-IR to millimeter spectral energy distributions (SEDs). These SEDs have a consistent shape, showing significantly higher mid-IR to submillimeter ratios than other galaxy templates, suggesting a hotter dust temperature.We estimate their dust temperatures to be 60-120 K using a single-temperature model. Their infrared luminosities are well over 10(exp 13) solar luminosity. These SEDs are not well fitted with existing galaxy templates, suggesting they are a new population with very high luminosity and hot dust. They are likely among the most luminous galaxies in the universe.We argue that they are extreme cases of luminous, hot dust-obscured galaxies (DOGs), possibly representing a short evolutionary phase during galaxy merging and evolution. A better understanding of their long-wavelength properties needs ALMA as well as Herschel data

Submarine Fernandina : magmatism at the leading edge of the Galapagos hot spot

Author Posting. © American Geophysical Union, 2006. This article is posted here by permission of American Geophysical Union for personal use, not for redistribution. The definitive version was published in Geochemistry Geophysics Geosystems 7 (2006): Q12007, doi:10.1029/2006GC001290.New multibeam and side-scan sonar surveys of Fernandina volcano and the geochemistry of lavas provide clues to the structural and magmatic development of Galápagos volcanoes. Submarine Fernandina has three well-developed rift zones, whereas the subaerial edifice has circumferential fissures associated with a large summit caldera and diffuse radial fissures on the lower slopes. Rift zone development is controlled by changes in deviatoric stresses with increasing distance from the caldera. Large lava flows are present on the gently sloping and deep seafloor west of Fernandina. Fernandina's submarine lavas are petrographically more diverse than the subaerial suite and include picrites. Most submarine glasses are similar in composition to aphyric subaerially erupted lavas, however. These rocks are termed the “normal” series and are believed to result from cooling and crystallization in the subcaldera magma system, which buffers the magmas both thermally and chemically. These normal-series magmas are extruded laterally through the flanks of the volcano, where they scavenge and disaggregate olivine-gabbro mush to produce picritic lavas. A suite of lavas recovered from the terminus of the SW submarine rift and terraces to the south comprises evolved basalts and icelandites with MgO = 3.1 to 5.0 wt.%. This “evolved series” is believed to form by fractional crystallization at 3 to 5 kb, involving extensive crystallization of clinopyroxene and titanomagnetite in addition to plagioclase. “High-K” lavas were recovered from the southwest rift and are attributed to hybridization between normal-series basalt and evolved-series magma. The geochemical and structural findings are used to develop an evolutionary model for the construction of the Galápagos Platform and better understand the petrogenesis of the erupted lavas. The earliest stage is represented by the deep-water lava flows, which over time construct a broad submarine platform. The deep-water lavas originate from the subcaldera plumbing system of the adjacent volcano. After construction of the platform, eruptions focus to a point source, building an island with rift zones extending away from the adjacent, buttressing volcanoes. Most rift zone magmas intrude laterally from the subcaldera magma chamber, although a few evolve by crystallization in the upper mantle and deep crust.This work was supported by the National Science Foundation grants OCE0002818 and EAR0207605 (D.G.), OCE0002461 (D.J.F. and M.K.), OCE9811504 (D.J.F. and M.R.P.), and EAR0207425 (K.H.) and WHOI postdoctoral support for Soule

The star formation history of BCGs to z = 1.8 from the SpARCS/SWIRE survey : evidence for significant in situ star formation at high redshift

We present the results of an MIPS-24 μm study of the brightest cluster galaxies (BCGs) of 535 high-redshift galaxy clusters. The clusters are drawn from the Spitzer Adaptation of the Red-Sequence Cluster Survey, which effectively provides a sample selected on total stellar mass, over 0.2 12) increases rapidly with redshift. Above z ∼ 1, an average of ∼20% of the sample have 24 μm inferred infrared luminosities of LIR > 1012 Lo, while the fraction below z ∼ 1 exhibiting such luminosities is <1%. The Spitzer-IRAC colors indicate the bulk of the 24 μm detected population is predominantly powered by star formation, with only 7/125 galaxies lying within the color region inhabited by active galactic nuclei (AGNs). Simple arguments limit the star formation activity to several hundred million years and this may therefore be indicative of the timescale for AGN feedback to halt the star formation. Below redshift z ∼ 1, there is not enough star formation to significantly contribute to the overall stellar mass of the BCG population, and therefore BCG growth is likely dominated by dry mergers. Above z ∼ 1, however, the inferred star formation would double the stellar mass of the BCGs and is comparable to the mass assembly predicted by simulations through dry mergers. We cannot yet constrain the process driving the star formation for the overall sample, though a single object studied in detail is consistent with a gas-rich merger.Peer reviewe