Designing and managing music festival experiences to enhance attendees’ psychological and social benefits

Attendance and participation at popular music festivals has become an important and increasingly common experience for people in many Western societies, yet little is known about the kinds of benefits visitors perceive they gain as a result of attending. This research explores attendees’ perceptions of the psychological and social benefits associated with their attendance of the Woodford Folk Music Festival in Queensland (Australia). Based upon the research findings, music festival management strategies are suggested to improve the design of festival experiences to better cater to the artistic, musical, social and psychological needs of attendees thereby increasing the impact and depth of the experience

A Review of Web-Based Job Advertisements for Australian Event Management Positions

Strong growths in the Australian event management industry, ongoing technological changes and the internationalisation of the market place has spurred the need for appropriately educated and trained event managers and for a re-evaluation of educational and job training curriculum to meet these new challenges. In order for Australia to position itself as a world leader in event management, it is important to provide consistent high professional standards and event managers that not only meet, but exceed the demands of the industry. While there is some literature that focuses on the tourism and leisure job market (Crossley, 1992; Keung & Pine, 2000), and a small but developing literature base that focuses on event management training (Harris & Jago, 1999; Hawkins & Goldbatt, 1995) relatively little consideration has been given to a national agenda for event management skilling. To provide an indication of current employer requirements, a nationwide study of job advertisements in event management has commenced. The aims of the study are to further the understanding of the educational needs and training requirements of the industry; to ascertain the learned skills and personal attributes sought from event managers; to determine the compatibility of industry demands with current educational and vocational provisions; and to suggest post-secondary institutional avenues through which event management education and training needs can be pursued. This is an ongoing study and it is hoped that it will contribute towards a broad scale understanding of the event management job market. More importantly however, it can be used as the basis for curriculum evaluation and training needs, and create a better understanding and compatibility between event management education and industry practice. This paper reports the preliminary results from a content analysis of approximately 100 web-based job advertisements. Email alert accounts were established with several search engines to gather a sample of event management related job advertisements from around Australia. An analytical framework was devised for the analysis of the advertisements themselves. The results reveal several interesting trends including the geographical concentration of the event management job market, the range of industries that require event management specialists or event management skills, and a series of required skills and key attributes of event managers. The results of this study establish a platform from which to develop a classification of event management skills required by the industry

Tormund's return: Hints of quasi-periodic eruption features from a recent optical tidal disruption event

Quasi-periodic eruptions (QPEs) are repeating thermal X-ray bursts associated with accreting massive black holes, the precise underlying physical mechanisms of which are still unclear. We present a new candidate QPE source, AT 2019vcb (nicknamed Tormund by the ZTF collaboration), which was found during an archival search for QPEs in the XMM-Newton archive. It was first discovered in 2019 as an optical tidal disruption event (TDE) at $z=0.088$, and its X-ray follow-up exhibited QPE-like properties. Our goals are to verify its robustness as QPE candidate and to investigate its properties to improve our understanding of QPEs. We performed a detailed study of the X-ray spectral behaviour of this source over the course of the XMM-Newton archival observation. We also report on recent Swift and NICER follow-up observations to constrain the source's current activity and overall lifetime, as well as an optical spectral follow-up. The first two Swift detections and the first half of the 30 ks XMM-Newton exposure of Tormund displayed a decaying thermal emission typical of an X-ray TDE. However, the second half of the exposure showed a dramatic rise in temperature (from 53 to 114 eV) and 0.2-2 keV luminosity (from $3.2\times10^{42}$ to $1.2\times10^{44}$ erg s$^{-1}$). The late-time NICER follow-up indicates that the source is still X-ray bright more than three years after the initial optical TDE. Although only a rise phase was observed, Tormund's strong similarities with a known QPE source (eRO-QPE1) and the impossibility to simultaneously account for all observational features with alternative interpretations allow us to classify Tormund as a candidate QPE. If confirmed as a QPE, it would further strengthen the observational link between TDEs and QPEs. It is also the first QPE candidate for which an associated optical TDE was directly observed, constraining the formation time of QPEs.Comment: Accepted for publication in A&A, 20 pages, 17 figure

O Corona, where art thou? eROSITA's view of UV-optical-IR variability-selected massive black holes in low-mass galaxies

Finding massive black holes (MBHs, $M_{BH}\approx10^4-10^7 M_{\odot}$) in the nuclei of low-mass galaxies ($M_{*}\lessapprox10^{10} M_{\odot}$) is crucial to constrain seeding and growth of black holes over cosmic time, but it is particularly challenging due to their low accretion luminosities. Variability selection via long-term photometric ultraviolet, optical, or infrared (UVOIR) light curves has proved effective and identifies lower-Eddington ratios compared to broad and narrow optical spectral lines searches. In the inefficient accretion regime, X-ray and radio searches are effective, but they have been limited to small samples. Therefore, differences between selection techniques have remained uncertain. Here, we present the first large systematic investigation of the X-ray properties of a sample of known MBH candidates in dwarf galaxies. We extracted X-ray photometry and spectra of a sample of $\sim200$ UVOIR variability-selected MBHs and significantly detected 17 of them in the deepest available \emph{SRG}/eROSITA image, of which four are newly discovered X-ray sources and two are new secure MBHs. This implies that tens to hundreds of LSST MBHs will have SRG/eROSITA counterparts, depending on the seeding model adopted. Surprisingly, the stacked X-ray images of the many non-detected MBHs are incompatible with standard disk-corona relations, typical of active galactic nuclei, inferred from both the optical and radio fluxes. They are instead compatible with the X-ray emission predicted for normal galaxies. After careful consideration of potential biases, we identified that this X-ray weakness needs a physical origin. A possibility is that a canonical X-ray corona might be lacking in the majority of this population of UVOIR-variability selected low-mass galaxies or that unusual accretion modes and spectral energy distributions are in place for MBHs in dwarf galaxies.Comment: Accepted for publication in A&

X-ray detection of a nova in the fireball phase

Novae are caused by runaway thermonuclear burning in the hydrogen-rich envelopes of accreting white dwarfs, which leads to a rapid expansion of the envelope and the ejection of most of its mass. Theory has predicted the existence of a ‘fireball’ phase following directly on from the runaway fusion, which should be observable as a short, bright and soft X-ray flash before the nova becomes visible in the optical. Here we report observations of a bright and soft X-ray flash associated with the classical Galactic nova YZ Reticuli 11 h before its 9 mag optical brightening. No X-ray source was detected 4 h before and after the event, constraining the duration of the flash to shorter than 8 h. In agreement with theoretical predictions, the source’s spectral shape is consistent with a black-body of 3.27 × 10 K (28.2 eV), or a white dwarf atmosphere, radiating at the Eddington luminosity, with a photosphere that is only slightly larger than a typical white dwarf.This work was supported by the Bundesministerium für Forschung und Technologie under DLR grants 50 QR 1603, 50 QR 2103 and 50 QR 2104. G.S. acknowledges support from the Spanish MINECO grant PID2020-117252GB-I00. V.S. thanks the Deutsche Forschungsgemeinschaft (DFG) for financial support (WE1312/53-1)

Winds of change: The nuclear and galaxy-scale outflows and the X-ray variability of 2MASS 0918+2117

Context. In this work, we test feedback propagation models on the test case of 2MASS 0918+2117 (2M0918), a z = 0.149 X-ray variable AGN that shows tentative evidence for nuclear ultra-fast outflows (UFOs) in a 2005 XMM-Newton observation. We also investigate whether UFOs can be related to the observed X-ray variability. Aims. We observed 2M0918 with XMM-Newton and NuSTAR in 2020 to confirm the presence of and characterize the UFOs. We performed a kinematic analysis of the publicly available 2005 SDSS optical spectrum to reveal and measure the properties of galaxy-scale ionized outflows. Furthermore, we constructed 20-year-long light curves of observed flux, line-of-sight column density, and intrinsic accretion rate from the spectra of the first four SRG/eROSITA all-sky surveys and archival observations from Chandra and XMM-Newton. Methods. We detect UFOs with v ~ 0.16c and galaxy-scale ionized outflows with velocities of ~700 km s-1. We also find that the drastic X-ray variability (factors > 10) can be explained in terms of variable obscuration and variable intrinsic luminosity. Results. Comparing the energetics of the two outflow phases, 2M0918 is consistent with momentum-driven wind propagation. 2M0918 expands the sample of AGN with both UFOs and ionized gas winds from 5 to 6 and brings the sample of AGN hosting multiscale outflows to 19, contributing to a clearer picture of feedback physics. From the variations in accretion rate, column density, and ionization level of the obscuring medium, we propose a scenario that connects obscurers, an accretion enhancement, and the emergence of UFOs

X-ray eruptions every 22 days from the nucleus of a nearby galaxy

Galactic nuclei showing recurrent phases of activity and quiescence have recently been discovered, with recurrence times as short as a few hours to a day -- known as quasi-periodic X-ray eruption (QPE) sources -- to as long as hundreds to a thousand days for repeating nuclear transients (RNTs). Here we report the discovery of Swift J023017.0+283603 (hereafter Swift J0230+28), a source that exhibits X-ray quasi-periodic eruptions from the nucleus of a previously unremarkable galaxy at $\sim$ 165 Mpc, with a recurrence time of approximately 22 days, an intermediary timescale between known RNTs and QPE sources. We also report transient radio emission from the source, which is likely associated with the X-ray eruptions. Such recurrent soft X-ray eruptions from a low-mass black hole, with no accompanying UV/optical emission are strikingly similar to QPE sources. However, in addition to having a recurrence time that is $\sim 25$ times longer than the longest-known QPE source, Swift J0230+28's eruptions exhibit slightly distinct shapes and temperature evolution than the known QPE sources. The observed properties disfavor disk instability models, and instead favor scenarios involving extreme mass ratio inspirals. Our discovery reveals a new timescale for repeating extragalactic transients and highlights the need for a wide-field, time-domain X-ray mission, which would enable the exploration of the parameter space of recurring X-ray transients.Comment: Under review on Nature Astronomy. Main Section: 14 pages, 3 figures and 1 Table. Methods: 32 pages, 11 Figures, 4 Table

Prospects for Time-Domain and Multi-Messenger Science with AXIS

The Advanced X-ray Imaging Satellite (AXIS) promises revolutionary science in the X-ray and multi-messenger time domain. AXIS will leverage excellent spatial resolution (<1.5 arcsec), sensitivity (80x that of Swift), and a large collecting area (5-10x that of Chandra) across a 24-arcmin diameter field of view to discover and characterize a wide range of X-ray transients from supernova-shock breakouts to tidal disruption events to highly variable supermassive black holes. The observatory's ability to localize and monitor faint X-ray sources opens up new opportunities to hunt for counterparts to distant binary neutron star mergers, fast radio bursts, and exotic phenomena like fast X-ray transients. AXIS will offer a response time of <2 hours to community alerts, enabling studies of gravitational wave sources, high-energy neutrino emitters, X-ray binaries, magnetars, and other targets of opportunity. This white paper highlights some of the discovery science that will be driven by AXIS in this burgeoning field of time domain and multi-messenger astrophysics.Comment: This White Paper is part of a series commissioned for the AXIS Probe Concept Mission; additional AXIS White Papers can be found at http://axis.astro.umd.ed

A new discovery space opened by eROSITA: Ionised AGN outflows from X-ray selected samples

Context. In the context of an evolutionary model, the outflow phase of an active galactic nucleus (AGN) occurs at the peak of its activity, once the central supermassive black hole (SMBH) is massive enough to generate sufficient power to counterbalance the potential well of the host galaxy. This outflow feedback phase plays a vital role in galaxy evolution. Aims. Our aim in this paper is to apply various selection methods to isolate powerful AGNs in the feedback phase, trace and characterise outflows in these AGNs, and explore the link between AGN luminosity and outflow properties. Methods. We applied a combination of methods to the Spectrum Roentgen Gamma (SRG) eROSITA Final Equatorial Depth survey (eFEDS) catalogue and isolated ∼1400 candidates at z &gt; 0.5 out of ∼11 750 AGNs (∼12%). Furthermore, we narrowed down our selection to 427 sources that have 0.5 &lt; z &lt; 1. We tested the robustness of our selection on the small subsample of 50 sources with available good quality SDSS spectra at 0.5 &lt; z &lt; 1 and, for which we fitted the [OIII] emission line complex and searched for the presence of ionised gas outflow signatures. Results. Out of the 50 good quality SDSS spectra, we identified 23 quasars (∼45%) with evidence of ionised outflows based on the presence of significant broad and/or shifted components in [OIII]λ5007 A. They are on average more luminous (log Lbol ∼ 45.2 erg s- 1) and more obscured (NH ∼ 1022 cm- 2) than the parent sample of ∼427 candidates, although this may be ascribed to selection effects affecting the good quality SDSS spectra sample. By adding 118 quasars at 0.5 &lt; z &lt; 3.5 with evidence of outflows reported in the literature, we find a weak correlation between the maximum outflow velocity and the AGN bolometric luminosity. On the contrary, we recovered strong correlations between the mass outflow rate and outflow kinetic power with the AGN bolometric luminosity. Conclusions. About 30% of our sample have kinetic coupling efficiencies, A /Lbol &gt; 1%, suggesting that the outflows could have a significant effect on their host galaxies. We find that the majority of the outflows have momentum flux ratios lower than 20 which rules out an energy-conserving nature. Our present work points to the unequivocal existence of a rather short AGN outflow phase, paving the way towards a new avenue to dissect AGN outflows in large samples within eROSITA and beyond

A case for a binary black hole system revealed via quasi-periodic outflows

Binaries containing a compact object orbiting a supermassive black hole are thought to be precursors of gravitational wave events, but their identification has been extremely challenging. Here, we report quasi-periodic variability in x-ray absorption, which we interpret as quasi-periodic outflows (QPOuts) from a previously low-luminosity active galactic nucleus after an outburst, likely caused by a stellar tidal disruption. We rule out several models based on observed properties and instead show using general relativistic magnetohydrodynamic simulations that QPOuts, separated by roughly 8.3 days, can be explained with an intermediate-mass black hole secondary on a mildly eccentric orbit at a mean distance of about 100 gravitational radii from the primary. Our work suggests that QPOuts could be a new way to identify intermediate/extreme-mass ratio binary candidates