tokens: taken with the Broadband Filter Imager, and the chromosphere, using the H α 6563 Å line obtained with the Visible Imaging Spectrometer (VIS). The passband of the TiO filter is 10 Å, centered at 7057 Å, while its temporal resolution is about 15 s with a pixel scale of 00343. Concerning VIS, a combination of 5 Å interference filter and a Fabry–Pérot etalon is used to get a bandpass of 0.07 Å at the H α line. Its field of view (FOV) is about 70′′ with a pixel scale of 00323. To obtain more spectral information, we scan the H α line at 11 positions with a 0.2 Å step following this sequence: ±1.0, ±0.8, ±0.6, ±0.4, ±0.2, 0.0 Å. The time used in each scan is 23 s. Both high-order adaptive optics (Cao et al. 2010 ) and a speckle reconstruction postprocessing method (KISIP speckle reconstruction code; Wöger von der Lühe 2007 ) are employed to achieve diffraction-limited resolution images. IRIS data are taken in a very large, coarse 64-step raster mode, with a step size of 035, step cadence of 31.8 s, and a raster cadence of 2036 s. The exposure time at each step is 29 s. Several strong emission lines are recorded, such as Si iv 1402.77 Å, Si iv 1393.7 Å, C ii 1334.53 Å, and Mg ii k 2796.35 Å. The cadences of the SJI in the passbands of 1400, 2796, and 2832 Å are all 112 s. The spatial resolution is about 033, and the FOV is 224 × 175′′ and 175′′ × 175′′ corresponding to the 64-step raster mode and the SJI. All of the spectra and images used in the analysis are level 2 data, including dark current subtraction and flat-field and geometrical corrections (De Pontieu et al. 2014 ; Tian et al. 2014 ). Hinode/SP data are acquired in a fast mode with an FOV of 81′′ × 81′′, a step size of 0297, and a raster cadence of 1080 s. Additionally, in order to analyze the corona response to our event, we have used SDO data, including the EUV and UV passbands from the AIA (Lemen et al. 2012 ) with cadences of 12 s and 24 s, respectively. The spatial register between the GST and SDO is first done by coaligning the AIA 1600 Å images with the GST/TiO data, and then coaligning the TiO data with the H α images at different wavelength positions. We use the AIA 1600 Å, IRIS 2832 Å, and SP continuum images to align the SDO , IRIS, and SP data. The uncertainty of the coalignment is about one AIA pixel (06). Figure 1 contains the context image of the LBs and fan-shaped jets on the sunspot of AR 12127 that we analyze in the subsequent section. The figure shows data from GST, IRIS, and SDO /AIA after the alignment process. Figure 1. Context images of the LBs and fan-shaped jets on the sunspot of AR 12127 obtained on 2014 August 1 around 17:27 UT. The different panels show (a) the photosphere through TiO images from GST, (b) the chromosphere via Ha LOS velocity obtained with GST/VIS, (c) the TR through SJI 1400 Å images from IRIS, and (d)–(i) the corona response observed with the different filters of SDO /AIA. R1 illustrates the LB region, to be analyzed in Figure 3 . L1 represents
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