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A key question in galaxy formation is how active galactic nuclei (AGN) interact with their host galaxies. Extremely Red Quasars (ERQs) are ideal objects to study this interaction since they are believed to be quasars caught in a short-lived phase where they are actively clearing gas from their host galaxy.s central regions. Most known ERQs are at z=2-3 comma making it challenging to resolve details of their winds and host galaxies comma even with HST. Here we propose to study the lowest redshift ERQ discovered to date (zvirgul0.94) with the aim of directly resolving the high ionization outflow using narrow-band imaging of the CORCHETE_OPENNe VCORCHETE_CLOSE line. The narrow band observations will provide a first look at the size and spatial distribution of a powerful quasar outflow during this key phase. The broad band observations will enable measurement of the host galaxy properties including Sersic index comma evidence of merging comma and recent (100 Myr) star formation. J0048-0046 provides the best possible chance to constrain the ionized gas outflow size of an ERQ comma both due to its low redshift and its high level of nuclear obscuration. With the derived outflow size measurements comma we can test our theories of galaxy formation and measure whether ERQ winds have enough kinetic power to blow the gas out of their hosts. These observations will also help contribute to building up a sample of ERQ hosts and outflow measurements that can be used to assess how ERQs outflows are driven and how the hosts of these galaxies evolve.

星系形成领域的核心问题之一，是活动星系核（active galactic nuclei, AGN）如何与其宿主星系产生相互作用。极红类星体（Extremely Red Quasars, ERQs）是研究该相互作用的理想天体，因为它们被认为是处于短暂演化阶段的类星体，此时正活跃地清除宿主星系中心区域的气体。目前已发现的极红类星体绝大多数处于红移z=2~3的区间，即便借助哈勃空间望远镜（Hubble Space Telescope, HST），也难以分辨其外流与宿主星系的细节结构。在此，我们拟研究迄今发现的红移最低的极红类星体（z≈0.94），目标是通过CORCHETE_OPENNe VCORCHETE_CLOSE谱线的窄带成像，直接解析其高电离外流。此次窄带观测将首次呈现该关键演化阶段中强大类星体外流的尺度与空间分布特征。宽带观测则可用于测量宿主星系的多项属性，包括塞斯克指数（Sersic index）、星系并合迹象，以及距今100 Myr（即1亿年）内的恒星形成活动。J0048-0046是目前约束极红类星体电离气体外流尺度的最佳候选天体，这一方面得益于其较低的红移，另一方面则因其核区存在较高的消光水平。通过获得的外流尺度测量结果，我们可以验证星系形成理论，并测算极红类星体的外流是否具备足够的动能将气体从宿主星系中吹出。此外，此次观测还将助力构建极红类星体宿主星系与外流测量的样本库，用于探究极红类星体外流的驱动机制，以及此类星系宿主的演化历程。