Purpose To assess US radiation oncologists’ views on practice scope and the ideal role of the radiation oncologist (RO), the American Society for Radiation Oncology (ASTRO) conducted a scope of practice survey. Methods and Materials In spring 2019, ASTRO distributed an online survey to 3822 US RO members. The survey generated 984 complete responses (26% response rate) for analysis. Face validity testing confirmed respondents were representative of ASTRO’s RO membership. Results Nearly all respondents agreed that “ROs should be leaders in oncologic care.” Respondents indicated the ideal approach to patient care was to provide “an independent opinion on radiation therapy and other treatment options” (82.5%) or “an independent opinion on radiation therapy but not outside of it” (16.1%), with only 1.4% favoring provision of “radiation therapy at the request of the referring physician” as the ideal approach. Actual practice fully matched the ideal approach in 18.2% of respondents. For the remaining majority, actual practice did not always match the ideal and comprised a mix of approaches that included providing radiation at the referring physician’s request 24.0% of the time on average. Reasons for the mismatch included fear of alienating referring physicians and concern for offering an unwelcome opinion. One-fifth of respondents expressed a desire to expand the scope of service though interspecialty politics and insufficient training were potential barriers. Respondents interested in expanding scope of practice were on average earlier in their career (average years in practice 13.3) than those who were not interested (average years in practice 17.2, P < .001). Radiopharmaceuticals administration, medical marijuana and anticancer medications prescribing, and RO inpatient service represented areas of interest for expansion but also knowledge gaps. Conclusions These results provide insight regarding US ROs’ scope of practice and attitudes on the ideal role of the RO. For most ROs, to provide an independent opinion on treatment options represented the ideal approach to care, but barriers such as concern of alienating referring physicians prevented many from fully adhering to their ideal in practice. Actual practice commonly comprised a mixed approach, including the least favored scenario of delivering radiation at the referring physician’s request one-quarter of the time, highlighting the influence of interspecialty politics on practice behavior. Advocacy for open communication and meaningful interdisciplinary collaboration presents an actionable solution toward a more balanced relationship with other specialties as ROs strive to better fulfill the vision of being leaders in oncologic care and being our best for our patients. The study also identified interest in expanding into nontraditional domains that offer opportunities to address unmet needs in the cancer patient’s journey and elevate radiation oncology within the increasingly value-based US health care system.
In "L. Campanelli, arXiv:1304.6534 [astro-ph.CO]", we have shown that cosmic magnetic fields are a natural consequence of inflation. Our results have been criticized in the recent comment "R. Durrer, G. Marozzi and M. Rinaldi, arXiv:1305.3192 [astro-ph.CO]." We show that the arguments raised against the validity of our results are physically and mathematically unfounded.
L. Spinoglio, M. Magliocchetti, S. Tommasin
et al.
SPECTROSCOPIC COSMOLOGICAL SURVEYS IN THE FAR-IR L. Spinoglio 1 , M. Magliocchetti 1 , S. Tommasin 1 , A. M. Di Giorgio 1 , C. Gruppioni 2 , G. De Zotti 3 , A. Franceschini 4 , M. Vaccari 4 , K. Isaak 5 , F. Pozzi 6 and M.A. Malkan 7 arXiv:0909.5044v1 [astro-ph.CO] 28 Sep 2009 Istituto di Fisica dello Spazio interplanetario - INAF, Via Fosso del Cavaliere 100, 00133 Roma, Italy Osservatorio Astronomico di Bologna - INAF, Via Ranzani 1, 40127, Bologna, Italy Osservatorio Astronomico di Padova - INAF, Vicolo dell’Osservatorio 5, 35122 Padova, Italy Dipartimento di Astronomia - Universit´ a di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy University of Cardiff - School of Physics and Astronomy, 5 The Parade, Cardiff CF24 3YB, United Kingdom Dipartimento di Astronomia - Universit´ a di Bologna - INAF, Via Ranzani 1, 40127, Bologna, Italy Astronomy Division, University of California, Los Angeles, CA 90095-1547, USA Abstract We show the feasibility of spectroscopic cosmological surveys with the SAFARI instrument onboard of SPICA. The work is done through simulations that make use of both empirical methods, i.e. the use of observed luminosity functions and theoretical models for galaxy formation and evolution. The relations assumed between the line emis- sion to trace AGN and star formation activity have been derived from the observations of local samples of galaxies. The results converge to indicate the use of blind spec- troscopy with the SAFARI FTS at various resolutions to study galaxy evolution from the local to the distant (z∼3) Universe. Specifically, two different and independent galaxy evo- lution models predict about 7-10 sources to be spectro- scopically detected in more than one line in a 2’× 2’ SA- FARI field of view, down to the expected flux limits of SAFARI, with about 20% of sources to be detected at z>2. SPICA-SAFARI will be therefore excellent at de- tecting high-z sources and at assessing in a direct way their nature (e.g whether mainly AGN or Star Formation powered) thanks to blind spectroscopy. correlation for active galaxies in the local Universe, as the two processes appear - at least in local Seyfert galaxies (Tommasin et al , 2009) to be almost independent of each other. The Magorrian relation therefore has to find its origins at earlier epochs. The study of galaxy evolution necessarily implies in- vestigation of the full cosmic history of energy generation by stars (star formation and stellar evolution) and black holes (accretion), as well as of the energy loss processes such as the feedback from AGNs, because all these are responsible for the build up of the baryonic mass in the Universe and must ultimately be consistent and set up the observed local relation between luminosity and mass in galaxies. To understand the Magorrian relation we need to make the cosmic connections between stars in a galaxy and its massive black hole. The global accretion power, measured at X-rays (Hasinger et al , 2005) and the star formation power, measured by Hα and rest-frame UV ob- servations (Shim et al , 2009) were ∼20 times higher at z=1-1.5 than today. On a cosmic scale, the evolution of supermassive black holes (SMBHs) appears related to the evolution of the star-formation rate (SFR), strongly sug- gesting the presence of co-evolution (Marconi et al , 2004; Key words: Galaxies: evolution, active galactic nuclei, star- Merloni et al , 2004; Shankar et al , 2009). As suggested by various authors (Heckman et al , 2004; Granato et al , burst – Missions: SPICA 2004), the growth of bulges through SF may be directly linked to the growth of black holes through accretion. Quasars have been advocated as a source of negative feed- 1. Introduction back that would quench star formation, however no clear In the last years our perspective of galaxy evolution has evidence for this ”negative feedback” has yet been found, greatly changed thanks to two main findings: A) the strong while instead star formation is often, although not al- correlation observed in the local Universe between the ways, concomitant with AGN/QSO activity over rather mass of the black hole at the centre of a galaxy and the long duty cycles (100 Myr - few 100 Myr). It has also been velocity dispersion of the stellar component of the galactic realized that the optically bright phase of quasars covers bulge (the so-called Magorrian relation), and B) the evi- not more than one tenth of their host lifetime, as obser- generally constrain quasar lifetimes to the range dence that most, if not all, galaxies during their evolution vations yr. Optical studies of local galaxies show that pass through a FIR/submillimetre bright phase. most, if not A) The Magorrian relation (Magorrian et al , 1998; Ferrarese & Merrit all, , large galaxy spheroids host massive relic black-holes (Richstone et al , 1998) which, in turn, sug- 2000) implies that the processes of black hole growth - gests that a mass-accreting AGN phase is one through through mass accretion - and bulge formation - through which all galaxies pass. star formation - are intimately linked. While large ellipti- cal galaxies with old stellar bulges are known to follow the Magorrian relation, we are not able to explain this tight B) To account for the total energy generated by stars and that by black hole accretion, one first has to determine Proc. Workshop ‘The Space Infrared Telescope for Cosmology & Astrophysics: Revealing the Origins of Planets and Galaxies’ 6–8 July 2009, Oxford, United Kingdom
We have undertaken an imaging survey of 34 nearby galaxies in far-ultraviolet (FUV, ∼1500 Å) and optical (UBVRI) passbands to characterize galaxy morphology as a function of wavelength. This sample, which includes a range of classical Hubble types from elliptical to irregular, with emphasis on spirals at low inclination angle, provides a valuable database for comparison with images of high-z galaxies whose FUV light is redshifted into the optical and near-infrared bands. Ultraviolet data are from the Ultraviolet Imaging Telescope (UIT) Astro-2 mission. We present images and surface brightness profiles for each galaxy, and we discuss the wavelength dependence of morphology for different Hubble types in the context of understanding high-z objects. In general, the dominance of young stars in the FUV produces the patchy appearance of a morphological type later than that inferred from optical images. Prominent rings and circumnuclear star formation regions are clearly evident in FUV images of spirals, while bulges, bars, and old, red stellar disks are faint to invisible at these short wavelengths. However, the magnitude of the change in apparent morphology ranges from dramatic in early-type spirals with prominent optical bulges to slight in late-type spirals and irregulars, in which young stars dominate both the UV and optical emission. Starburst galaxies with centrally concentrated, symmetric bursts display an apparent "E/S0" structure in the FUV, while starbursts associated with rings or mergers produce a peculiar morphology. We briefly discuss the inadequacy of the optically defined Hubble sequence in describing FUV galaxy images and estimating morphological k-corrections, and we suggest some directions for future research with this data set.
(Abbreviated) We present an imaging survey of 37 nearby galaxies observed with HST/WFPC2 in the mid-UV F300W filter and in F814W. 11 galaxies were also imaged in F255W. These galaxies were selected to be detectable with WFPC2 in one orbit, and cover a wide range of Hubble types and inclinations. The mid-UV spans the gap between our groundbased optical/NIR images and far-UV images available from the Astro/UIT missions. Our first qualitative results are: (1) Early-type galaxies show a significant decrease in surface brightness going from the red to the mid-UV, and in some cases the presence of dust lanes. Some galaxies would be classified different when viewed in the mid-UV, some become dominated by a blue nuclear feature or point source. (2) Half of the mid-type spiral and star-forming galaxies appear as a later morphological type in the mid-UV, as Astro/UIT also found in the far-UV. Some- times these differences are dramatic. The mid-UV images show a considerable range in the scale and surface brightness of individual star-forming regions. Almost all mid-type spirals have their small bulges bi-sected by a dust-lane. (3) Most of the heterogeneous subset of late-type, irregular, peculiar, and merging galaxies display F300W morphologies that are similar to those seen in F814W, but with differences due to recognizable dust features absorbing the bluer light, and due to UV-bright hot stars, star-clusters, and star-forming ridges. In the rest-frame mid-UV, early- to mid-type galaxies are more likely to be misclassified as later types than vice versa. This morphological K-correction explains only part of the excess faint blue galaxies seen in deep HST fields.
The title compound, which may be prepared from C5H5(CO)2Mn—P(Ph)Cl2 and Fe2(CO)9 crystallizes in the monoclinic space group C 2/c with a = 1579(2), b = 1592(2), c = 1790(3) pm, β = 97.2(1)°, Z = 8. The structure was solved by direct methods. Full matrix refinement led to R1= 0.066. The compound contains a threemembered metallocycle with two iron and one manganes atoms. Each iron atom bears three terminal carbonyl groups; the two CO-ligands of the C5H5Mn(CO)2 fragment form unsymmetrical bridges with the two iron atoms. The metal triangel is capped by a Ph—P group with a triply bridging phosphorus atom.
We discuss far-UV (FUV) (1500 Å) surface photometry and FUV-B color profiles for eight E/S0 galaxies from images taken with the Ultraviolet Imaging Telescope, primarily during the Astro-2 mission. In three cases, the FUV radial profiles are more consistent with an exponential than a de Vaucouleurs function, but there is no other evidence for the presence of a disk or of young, massive stars. In all cases except M32, the FUV-B color becomes redder at larger radii. There is a wide range of internal radial FUV-B color gradients. However, we find no correlation between the FUV-B color gradients and internal metallicity gradients based on Mg absorption features. We conclude that metallicity is not the sole parameter controlling the "UV upturn component" in old populations.
Far-UV (wavelength 1520 Å), U, Hα, and R images of the interacting Sbc spiral galaxy M51 were obtained by the Ultraviolet Imaging Telescope (UIT) during the Astro-2 Spacelab mission of 1995 March and at Mount Laguna Observatory. The μ152 - μU radial gradient of over 1 mag, becoming bluer with increasing radius, is attributed primarily to a corresponding radial extinction gradient. Magnitudes in both UV bands and Hα fluxes are reported for 28 H II regions. Optical extinctions for the 28 corresponding UV sources are computed from the measured m152 - U colors by fitting to the optical extinctions of Nakai & Kuno. The estimated normalized far-UV extinction A152/E(B-V) increases with increasing Galactocentric distance (decreasing metallicity), from 5.99 to 6.54, compared with the Galactic value 8.33. The best-fit m152 - U color for no extinction, -3.07, is the color of a model solar metallicity starburst of age ~2.5 Myr with IMF slope -1.0. H II regions show decreasing observed Hα fluxes with decreasing radius, relative to the Hα fluxes predicted from the observed f152 for age 2.5 Myr, after the Hα and f152 are corrected for extinction. We attribute the increasing fraction of “missing” Hα flux with decreasing radius to increasing extinction in the Lyman continuum. The increasing extinction-corrected far-UV flux of the H II regions with decreasing distance to the nucleus is probably a result of the corresponding increasing column density of the interstellar gas resulting in larger mass OB associations. The estimated dust-absorbed Lyman continuum energy flux is ~0.6 times the far-infrared energy flux of M51 observed by IRAS.
We present a 1620 Å image of the nearby globular cluster NGC 6752 obtained with the Ultraviolet Imaging Telescope (UIT) during the Astro-2 mission of the Space Shuttle Endeavour in 1995 March. An ultraviolet-visible color-magnitude diagram (CMD) is derived for 216 stars matched with the visible photometry of Buonanno et al. This CMD provides a nearly complete census of the hot horizontal-branch (HB) population with good temperature and luminosity discrimination for comparison with theoretical tracks. The observed data show good agreement with the theoretical zero-age horizontal branch (ZAHB) of Sweigart for an assumed reddening of E(B - V) = 0.05 and a distance modulus of 13.05. The observed HB luminosity width is in excellent agreement with the theoretical models and supports the single-star scenario for the origin of extreme horizontal branch (EHB) stars. However, only four stars can be identified as post-EHB stars, whereas almost three times this many are expected from the HB number counts. If this effect is not a statistical anomaly, then some noncanonical effect may be decreasing the post-EHB lifetime. The recent noncanonical models of Sweigart, which have helium-enriched envelopes due to mixing along the red giant branch, cannot explain the deficit of post-EHB stars, but might be better able to explain their luminosity distribution.