Reforming fossil fuel subsidies provides opportunity to better target government support towards women and children

A new report from the Global Subsidies Initiative of the International Institute for Sustainable Development (IISD) finds that Bangladeshi, Indian and Nigerian governments can significantly curb poverty among women and children in their countries by redesigning fossil fuel subsidie

Mapping India's Energy Policy 2022

Carefully designed energy support measures—subsidies, public utilities' investments, and public finance institutions' lending—and government's energy revenues play a key role in India's transition to clean energy and reaching net-zero emissions by 2070. Looking at how the Government of India has supported different types of energy from FY 2014 to FY 2021, the study aims to improve transparency, create accountability, and encourage a responsible shift in support away from fossil fuels and toward clean energy.Mapping India's Energy Subsidies 2022 covers India's subsidies to fossil fuels, electricity transmission and distribution, renewable energy, and electric vehicles between fiscal year (FY) 2014 and FY 2021.We found that fossil fuels continue to receive far more subsidies than clean energy in India. This disparity became even more pronounced from FY 2020 to FY 2021, going from 7.3 times to 9 times the amount of subsidies to renewables

Mapping India's energy subsidies 2021: time for renewed support to clean energy.

Government support is more important than ever for the energy transition in the wake of COVID-19, as governments around the world take unprecedented measures to help stimulate economic recovery. Shifting government support from fossil to clean energy can ensure that every rupee of public money helps access, affordability, energy security and the shift to a low-carbon economy. This report examines how the Government of India has used subsidies to support different types of energy from FY 2014 until FY 2020, and draws on qualitative data to describe major shifts since the onset of COVID-19. In light of the government commitments to Aatmanirbhar Bharat ("self-reliant India"), it also includes two special thematic chapters. The first explores how subsidy policy can best promote solar photovoltaic (PV) manufacturing as part of the road to 450 GW of renewable energy by 2030. The second examines how investments by public sector undertakings (PSUs) - that is, enterprises where the government is the majority owner - are supporting clean energy. Our data, summarized in Figure ES1, cover all subsidies from production to consumption for coal, oil and gas, electricity transmission and distribution (T&D), renewable energy, and electric vehicles (EVs). Nuclear and hydropower are not included due to a lack of adequate data availability. The underlying data are available online and have been made easier to explore with an accompanying data portal

Cloud System Evolution in the Trades (CSET): Following the Evolution of Boundary Layer Cloud Systems with the NSFNCAR GV

The Cloud System Evolution in the Trades (CSET) study was designed to describe and explain the evolution of the boundary layer aerosol, cloud, and thermodynamic structures along trajectories within the North Pacific trade winds. The study centered on seven round trips of the National Science FoundationNational Center for Atmospheric Research (NSFNCAR) Gulfstream V (GV) between Sacramento, California, and Kona, Hawaii, between 7 July and 9 August 2015. The CSET observing strategy was to sample aerosol, cloud, and boundary layer properties upwind from the transition zone over the North Pacific and to resample these areas two days later. Global Forecast System forecast trajectories were used to plan the outbound flight to Hawaii with updated forecast trajectories setting the return flight plan two days later. Two key elements of the CSET observing system were the newly developed High-Performance Instrumented Airborne Platform for Environmental Research (HIAPER) Cloud Radar (HCR) and the high-spectral-resolution lidar (HSRL). Together they provided unprecedented characterizations of aerosol, cloud, and precipitation structures that were combined with in situ measurements of aerosol, cloud, precipitation, and turbulence properties. The cloud systems sampled included solid stratocumulus infused with smoke from Canadian wildfires, mesoscale cloudprecipitation complexes, and patches of shallow cumuli in very clean environments. Ultraclean layers observed frequently near the top of the boundary layer were often associated with shallow, optically thin, layered veil clouds. The extensive aerosol, cloud, drizzle, and boundary layer sampling made over open areas of the northeast Pacific along 2-day trajectories during CSET will be an invaluable resource for modeling studies of boundary layer cloud system evolution and its governing physical processes

Discovery and Early Evolution of ASASSN-19bt, the First TDE Detected by TESS

We present the discovery and early evolution of ASASSN-19bt, a tidal disruption event (TDE) discovered by the All-Sky Automated Survey for Supernovae (ASAS-SN) at a distance of $d\simeq115$ Mpc and the first TDE to be detected by TESS. As the TDE is located in the TESS Continuous Viewing Zone, our dataset includes 30-minute cadence observations starting on 2018 July 25, and we precisely measure that the TDE begins to brighten $\sim8.3$ days before its discovery. Our dataset also includes 18 epochs of Swift UVOT and XRT observations, 2 epochs of XMM-Newton observations, 13 spectroscopic observations, and ground data from the Las Cumbres Observatory telescope network, spanning from 32 days before peak through 37 days after peak. ASASSN-19bt thus has the most detailed pre-peak dataset for any TDE. The TESS light curve indicates that the transient began to brighten on 2019 January 21.6 and that for the first 15 days its rise was consistent with a flux $\propto t^2$ power-law model. The optical/UV emission is well-fit by a blackbody SED, and ASASSN-19bt exhibits an early spike in its luminosity and temperature roughly 32 rest-frame days before peak and spanning up to 14 days that has not been seen in other TDEs, possibly because UV observations were not triggered early enough to detect it. It peaked on 2019 March 04.9 at a luminosity of $L\simeq1.3\times10^{44}$ ergs s$^{-1}$ and radiated $E\simeq3.2\times10^{50}$ ergs during the 41-day rise to peak. X-ray observations after peak indicate a softening of the hard X-ray emission prior to peak, reminiscent of the hard/soft states in X-ray binaries.Comment: 23 pages, 14 figures, 5 tables. A machine-readable table containing the host-subtracted photometry presented in this manuscript is included as an ancillary fil

Stratospheric Gravity Wave Fluxes and Scales during DEEPWAVE

During the Deep Propagating Gravity Wave Experiment (DEEPWAVE) project in June and July 2014, the Gulfstream V research aircraft flew 97 legs over the Southern Alps of New Zealand and 150 legs over the Tasman Sea and Southern Ocean, mostly in the low stratosphere at 12.1-km altitude. Improved instrument calibration, redundant sensors, longer flight legs, energy flux estimation, and scale analysis revealed several new gravity wave properties. Over the sea, flight-level wave fluxes mostly fell below the detection threshold. Over terrain, disturbances had characteristic mountain wave attributes of positive vertical energy flux (EFz), negative zonal momentum flux, and upwind horizontal energy flux. In some cases, the fluxes changed rapidly within an 8-h flight, even though environmental conditions were nearly unchanged. The largest observed zonal momentum and vertical energy fluxes were MFx = −550 mPa and EFz = 22 W m−2, respectively. A wide variety of disturbance scales were found at flight level over New Zealand. The vertical wind variance at flight level was dominated by short “fluxless” waves with wavelengths in the 6–15-km range. Even shorter scales, down to 500 m, were found in wave breaking regions. The wavelength of the flux-carrying mountain waves was much longer—mostly between 60 and 150 km. In the strong cases, however, with EFz \u3e 4 W m−2, the dominant flux wavelength decreased (i.e., “downshifted”) to an intermediate wavelength between 20 and 60 km. A potential explanation for the rapid flux changes and the scale “downshifting” is that low-level flow can shift between “terrain following” and “envelope following” associated with trapped air in steep New Zealand valleys

The Carnegie-Chicago Hubble Program. VIII. An Independent Determination of the Hubble Constant Based on the Tip of the Red Giant Branch

We present a new and independent determination of the local value of the Hubble constant based on a calibration of the tip of the red giant branch (TRGB) applied to Type Ia supernovae (SNe Ia). We find a value of H0 = 69.8 ± 0.8 (±1.1% stat) ± 1.7 (±2.4% sys) km s−1 Mpc−1. The TRGB method is both precise and accurate and is parallel to but independent of the Cepheid distance scale. Our value sits midway in the range defined by the current Hubble tension. It agrees at the 1.2σ level with that of the Planck Collaboration et al. estimate and at the 1.7σ level with the Hubble Space Telescope (HST) SHoES measurement of H0 based on the Cepheid distance scale. The TRGB distances have been measured using deep HST Advanced Camera for Surveys imaging of galaxy halos. The zero-point of the TRGB calibration is set with a distance modulus to the Large Magellanic Cloud of 18.477 ± 0.004 (stat) ± 0.020 (sys) mag, based on measurement of 20 late-type detached eclipsing binary stars, combined with an HST parallax calibration of a 3.6 μm Cepheid Leavitt law based on Spitzer observations. We anchor the TRGB distances to galaxies that extend our measurement into the Hubble flow using the recently completed Carnegie Supernova Project I ( CSP-I ) sample containing about 100 well-observed SNe Ia . There are several advantages of halo TRGB distance measurements relative to Cepheid variables; these include low halo reddening, minimal effects of crowding or blending of the photometry, only a shallow (calibrated) sensitivity to metallicity in the I band, and no need for multiple epochs of observations or concerns of different slopes with period. In addition, the host masses of our TRGB host-galaxy sample are higher, on average, than those of the Cepheid sample, better matching the range of host-galaxy masses in the CSP-I distant sample and reducing potential systematic effects in the SNe Ia measurements

The Carnegie-Chicago Hubble Program. VIII. An Independent Determination of the Hubble Constant Based on the Tip of the Red Giant Branch

We present a new and independent determination of the local value of the Hubble constant based on a calibration of the Tip of the Red Giant Branch (TRGB) applied to Type Ia supernovae (SNeIa). We find a value of Ho = 69.8 +/- 0.8 (+/-1.1\% stat) +/- 1.7 (+/-2.4\% sys) km/sec/Mpc. The TRGB method is both precise and accurate, and is parallel to, but independent of the Cepheid distance scale. Our value sits midway in the range defined by the current Hubble tension. It agrees at the 1.2-sigma level with that of the Planck 2018 estimate, and at the 1.7-sigma level with the SHoES measurement of Ho based on the Cepheid distance scale. The TRGB distances have been measured using deep Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) imaging of galaxy halos. The zero point of the TRGB calibration is set with a distance modulus to the Large Magellanic Cloud of 18.477 +/- 0.004 (stat) +/-0.020 (sys) mag, based on measurement of 20 late-type detached eclipsing binary (DEB) stars, combined with an HST parallax calibration of a 3.6 micron Cepheid Leavitt law based on Spitzer observations. We anchor the TRGB distances to galaxies that extend our measurement into the Hubble flow using the recently completed Carnegie Supernova Project I sample containing about 100 well-observed SNeIa. There are several advantages of halo TRGB distance measurements relative to Cepheid variables: these include low halo reddening, minimal effects of crowding or blending of the photometry, only a shallow (calibrated) sensitivity to metallicity in the I-band, and no need for multiple epochs of observations or concerns of different slopes with period. In addition, the host masses of our TRGB host-galaxy sample are higher on average than the Cepheid sample, better matching the range of host-galaxy masses in the CSP distant sample, and reducing potential systematic effects in the SNeIa measurements.Comment: 60 pages, 20 figures, accepted for publication in the Astrophysical Journa

Lee Silverman Voice Treatment versus NHS Speech and Language Therapy versus control for dysarthria in Parkinson’s disease (PD COMM):a UK, multicentre, pragmatic, randomised controlled trial

Objectives: We aimed to assess the clinical effectiveness of two speech and language therapy (SLT) approaches versus no speech and language therapy for dysarthria in people with Parkinson’s disease. Design: This was a pragmatic, UK-wide, multicentre, three-arm, parallel group, unblinded, randomised controlled trial. Participants were randomly assigned using minimisation in a 1:1:1 ratio to Lee Silverman Voice Treatment (LSVT LOUD®), NHS SLT, or no SLT. Analyses were based on the intention to treat principle.Setting: The speech and language therapy interventions were delivered in outpatient or home settings.Participants: Between September 2016 and March 2020, 388 people with Parkinson’s disease and dysarthria were randomised into the trial: 130 to LSVT LOUD®, 129 to NHS SLT, and 129 to no SLT.Interventions: Lee Silverman Voice Treatment (LSVT LOUD®) consisted of four, face-to-face or remote, 50-minute sessions each week delivered over 4 weeks. Home-based practice activities were set for up to 5 to 10 minutes daily on treatment days and 15 minutes twice daily on non-treatment days. NHS Speech and language therapy (NHS SLT) dosage was determined by the local therapist in response to individual participants’ needs. Prior research suggested that NHS SLT participants would receive an average of one session per week over 6 to 8 weeks. Local practices for NHS SLT were accepted, except for those within the LSVT LOUD® protocol. Main outcome measures: The primary outcome was the self-reported Voice Handicap Index (VHI) total score at 3 months.Results: People randomised to LSVT LOUD® reported lower VHI scores at 3 months post-randomisation than those who were randomised to no SLT (-8·0 points (99%CI: -13·3 to -2·6); p = 0·0001). There was no evidence of a difference in VHI scores between NHS SLT and no SLT (1·7 points; (99%Cl: -3·8 to 7·1); p = 0·43). Patients randomised to LSVT LOUD® also reported lower VHI scores than those randomised to NHS SLT (-9·6 points; (99%CI: -14·9 to -4·4); p &lt; 0.0001). There were 93 adverse events (predominately vocal strain) in the LSVT LOUD® group, 46 in the NHS SLT group, and none in the no SLT group. There were no serious adverse events. Conclusions: LSVT LOUD® was more effective at reducing the participant reported impact of voice problems than no SLT and NHS SLT. NHS SLT showed no evidence of benefit compared to no SLT. Trial registration: The completed trial registration is ISRCTN12421382. Funding: NIHR HTA Programme, project number HTA 10/135/02. <br/